modelling agencies europe

© 2024 MODELS 1 LIMITED. ALL RIGHTS RESERVED.

TERMS & CONDITIONS \ PRIVACY POLICY \ DATA PROTECTION

MEDIASLIDE MODEL AGENCY SOFTWARE

DESIGNED BY SHOCK!

• Development
• Men Development
• Terms & conditions
• Model Polaroids
• Become a model

Top 11 International Modeling Agencies + 44 Top Models

International modeling is a rewarding career because it offers many different options, like traveling the world and working with some of the best designers and photographers.

In fact, international models from around the world including Europe, Asia, and America, often find that their jobs abroad were the stepping stones that led them to more prestigious fashion jobs in top markets like: New York, Los Angeles, Chicago, and Miami.

HOW DO YOU BECOME AN INTERNATIONAL MODEL?

There are plenty of ways that people have tried and succeeded. Here’s a list of some international modeling agencies that develop top models. You should consider applying to the agencies listed below!

WHAT DO YOU NEED BEFORE YOU GO OVERSEAS?

WHO WILL PAY FOR YOUR EXPENSES?

WHERE WILL YOU STAY?

DO YOU GET AN ALLOWANCE?

HOW MUCH COMMISSION WILL YOUR AGENT RECIEVE?

HOW WILL YOU NAVIGATE IN A NEW COUNTRY?

WHAT IF YOU DON’T SPEAK THE NATIVE LANGUAGE?

WATCH THE VIDEO TO FIND OUT MORE!

1. CHIC MANAGEMENT

Chic Management is an international modeling agency specializing in the representation of international models, who want to travel and represent top fashion brands in Australia and around the world.

They cater to a range of different clients who come to them from around the globe with varying projects. CHIC  has established itself as a leading agency in the fashion industry, and upholds a reputation of integrity and professionalism.

CHIC aims to bring the best models in the world to Australia to represent all sectors.

The agency has a strong network of contacts in the industry. Their models are known to book work for top editorial magazines like:

• Vogue Portugal

• Marie Claire Australia

• RUSSH Magazine

They have an impressive roster of clients in the industry such as:

• Aje Clothing

Established in 1992, Chic Management continues to grow their network by working with leading clients and models in the fashion industry.

2. FANCINA MODELS

Francina Models is one of the leading international agencies in Barcelona, Spain, representing models from all over the world.

You may be surprised to know that Barcelona, Spain is home to some of the top fashion models in the world. The agency  represents models of many sizes and ethnicities, from all over the world.

As an international modeling agency in Barcelona, Francina Models is committed to working with a strong roaster of men and women to create a portfolio that will bring them to the top.

As Francina Models continues to dominate Barcelona as a leading agency, you can find their models working for clients like: 

• H&M innovation campaign
• Paloma Wool

So if you’re looking for an international model agency in Barcelona, Spain, look no further.

VIEW THEIR PORTFOLIO

IB RAHIMA_D

3. FORD MODELS BRASIL

Ford Models Brazil is a full-service modeling agency with an extensive portfolio of international models.

They take pride in their work by presenting a broad experience in the fashion industry; with professional models that work directly with major brands, advertising agencies, and media and production companies.

Ford Models Brazil has been providing its clients with high-quality services.  In addition, it has managed to build a reputation for itself by having many successful campaigns, especially in the commercial advertising market.

Ford Brasil has an exclusive men’s and women’s board, that represents models of all types of people such as: 

• Full figured

• Over 30 Years Old

• Influencers on Social Media

Ford Models Brasil is known for continuously booking their models with world re-owned brands like,

• Harper’s Bazaar España
• Marc Jacobs
• LANÇA PERFUME
• Vult Beauty and Cosmetics

Give Ford Models Brasil a try!

4. SCOOP MODELS - COPENHAGEN

Scoop Models is the leading modeling agency in Copenhagen, Denmark. Scoop Models Copenhagen has a very clear vision and business model.

Scoop focuses on working with a diverse group of models from all over the world, educating others, and changing the negative stereotypes about beauty and gender identity.

The agency houses top fashion models like:

• Cara Delevingne

• Prince Nikoli

Scoop Models has three main pillars:

1. To help models reach a better position within the fashion industry.

2. To provide the best training and development

3. To provide the best customer service to clients

Their models are known are known to travel internationally for fashion week in:

• Paris Fashion Week
• Milan Fashion Week
• London Fashion Week
• New York Fashion Week
• Nensi Dojaka
• Khaite New York

If you’re ready to get scouted, get in touch with Scoop Models by following the agency on social media and filling out a model application.

5. M4 MODELS - GERMANY

Based in Germany with offices in Hamburg and Berlin, M4 Models is a full serve modeling agency that represents familiar international models that are known to be the fashion industries top models.

They believe in building reputable relationships with inspiring brands that stand for something meaningful. The success of the agency, makes their models and clients proud of being associated with them.

Their goal is to find the perfect model for the right job. That’s why they take a lot of time and effort to scout the right models for the right clients.

Their models book jobs with exciting clients like:

• Numero Thailand
• Rollercoaster Magazine
• Gucci Beauty Wish Campaign

Are you looking for a German modeling agency to help you work for reputable brands and magazines?

Look no further, apply to M4 scouts!

6. IMAGE - TOKYO

Image Models is a boutique agency with an international focus. They represent mainly Japanese women, but also have a handful of women and men from other countries.

The two biggest areas of their focus are fashion and beauty. Their clients range from top designers to magazine brands.

Their models are known to grace the covers of:

• GQ Magazine
• Fudge Magazine

Their models are known to work with brands like:

• GISELe Magazine
• Champion Japan

The agency is always open for submissions from models.

APPLY HERE  or Email:    [email protected]

7. SELECT MODELS - STOCKHOLM

Select Models’ network includes some of the biggest names in fashion. The agency is known to represent a strong roaster of top models and unique faces in development.

Editorial model Abény Nhial, is signed to Select Models. She has helped shift the industry forward with her appearance on the cover of British Vogue’s All African Cover.

Select is known for their extensive background in fashion, commercial, editorial campaigns – nationally and internationally.

Their models have also worked with big brands like:

• Louis Vuitton
• 5’ ELEVEN’’ Magazine
• ODDA Magazine

Located in Stockholm, Sweden, the agency consists of a team of experienced professionals who help their clients develop and promote their brands. They represent and manage models in all areas of fashion, commercial, runway and beauty.

8. ESEE MODEL MANAGEMENT - SHANGHAI

Esee models was established in Canada and successfully gained clients all over the world. G aining a good reputation with clients and the trust of models, the agency believed it would be a good idea to open an office in Shanghai, China.

As a result of that major shift, Esee models has the most experienced international modeling agency in East China.

Esee’s business model is simple: every model that’s signed to their agency has sufficient modeling experience in many countries like Milan, Paris, Tokyo, Seoul, and Hong Kong.

Their goal is to provide the best services to fashion brands, as well as keeping their models constantly working with the latest fashion trends.

Here’s a list of brands that the agency is known to frequently book their models with:

• Karl Lagerfeld
• Marie Claire China
• BAZAAR MEN China

Esee Models is an international management worth applying to!

APPLY HERE  

9. ELITE MODELS - PARIS

Elite Paris founded by John Casablancas, whose also famous for having a modeling school. The international modeling agency originated in Paris, France and later expanded their network in New York, Los Angeles, Miami, London and Toronto.

As an international modeling agency, Elite is one of the first agencies to go beyond a basic representation agreement, giving their models career management, health and wellness guidance and the support and security that comes with a powerful global network.

Elite Paris represents runway and print clients, and has a proven track record of representing high-profile models like:

Adesuwa, Adriana Lima, Fisher Smith, and Jin Dachuan.

Elites’ models are known to work with clients like:

• Elle Poland
• Lampoon Magazine
• De Beers “The Alchemist of Light” Campaign

What are you waiting for? Give Elite Models Paris a shot!

10. IMG LONDON

IMG Models offers a diverse client roster that spans the fashion, beauty, and entertainment industries.

The London office prides itself on its ability to consistently find and develop fresh faces and models for its UK clients.

From aspiring models to established professionals, IMG models helps their clients discover the perfect fit for their brand and marketing material.

Their models have extensive experience in runway, magazine work, advertising campaigns, editorials, and commercial shoots.

They provide full service, and manage everything from scouting, casting, talent acquisition, and contract negotiation to production and post-production.

Their models have graced the covers and pages of famous magazines like:

• Document Magazine
• Crosscurrent
• CircleZeroEight
• British vogue

They seek both men and women who represent the diversity of modern beauty, with a focus on high fashion and athleticism.

APPLY HERE   

11. WHY NOT MODELS - MILAN

Why Not Models is an international agency with offices in Milan and New York. Their core expertise lies in the area of fashion, where they have many years of experience.

Why Not Models aim is to continue to grow a network of fashion professionals, by providing both clients and models with a successful experience that will help grow their image.

Why Not provides the best models to advertising agencies, producers, photographers, and designers.

They have extensive experience in Milan Fashion Week and have worked in the past with many designers such as:

• BVLGARI Official
• Armani Exchange
• Vogue Arabia

Home of top notch supermodels, Why Not Models Milan is an agency you should consider.

APPLY HERE 

3 thoughts on “Top 11 International Modeling Agencies + 44 Top Models”

What about MandP Models UK?

Yes! Located in London, they’re an awesome agency to submit to!! If you’re not located in London I would e-mail them first and ask if they accept submission from your location! If you need any additional modeling tips you can email me or submit through the Mentorship form! <3

HeLlo! I want to know if you accept submissions from Switzerland. My name is Yolanda and I am a model from Argentina, currently living in Basel.

Leave a Comment Cancel Reply

Your email address will not be published. Required fields are marked *

Save my name, email, and website in this browser for the next time I comment.

Nikita Gnetnev walks Dior SS25

Nikita Gnetnev walks Wooyoungmi SS25

Nikita Gnetnev walks Kolor SS25

Nikita Gnetnev walks Undercover SS25

Magnus Tanggaard walks Sean Suen SS25

Nikita Gnetnev walks Songzio SS25

Nikita Gnetnev debuts for Prada SS25

Magnus Tanggaard walks Dolce & Gabbana SS25

Magnus Tanggaard walks Neil Barrett SS25

Magnus Tanggaard walks Moschino SS25

Edmilson Tavares for L'officiel Hommes Belgium shot by Daniella Rodrigues

Clement Chabernaud for Gucci FW24 Men's Campaign shot by David Sims

Giedre Dukauskaite covers Mia Le Journal shot by Adriano Russo

Vivien Solari for British Vogue shot by Emma Tempest

Rui Huila for LOEWE x Mytheresa

Mukasa Kakonge for Polo Ralph Lauren

Kathie Lam for Vero Moda

Zoe Barnard covers Harper's Bazaar UK shot by David Roemer

Valdemar Buch for Café shot by Sara Bille

Maggie Maurer for Vogue Portugal shot by Alessio Albi

Cate Underwood for Elle France shot by Gilad Sasporta

SHOWCAST modeling agency

We cast, book and place models, actors and influencers for projects in Germany and Europe.

As a modeling agency with a focus on medium-sized businesses, we have been offering efficient, reputable and reliable services to customers from all over Europe since 2010. Our international model pool offers diversity with best-agers, people, curvy and plus-size models as well as models for sports, fitness and lifestyle productions.  With castings in our studio in Cologne as well as in Berlin, Hamburg and Munich, we are your modeling agency in Germany.

At SHOWCAST, we understand the dynamics of digital marketing. In addition to traditional model booking, we offer strategic and campaign-related influencer marketing. We commission creators to produce your UGC media. Our optimized workflows guarantee smooth processing and ensure that your campaign visions are implemented authentically and effectively.

Als Modelagentur mit Sitz in Köln sind wir bundesweit aktiv und bieten erfolgreiche Projektbesetzungen in Deutschland und Europa. Unsere Kunden sind Fotografen, Werbe- und PR-Agenturen, die Wert auf authentische Kommunikation legen, Modehäuser, die trendgerecht und stilsicher verkaufen, sowie Unternehmen, die effizient Videos und Fotos für ihr E-Commerce produzieren. Wir sind Ansprechpartner für Mode-, Beauty- und Lifestyle-Influencer-Marketing. Unser Ziel ist es, eure Kreationen zeitgemäß und wirkungsvoll zu präsentieren. Dank regelmäßiger Castings in Köln und in vielen Großstädten Deutschlands sowie einem umfangreichen Netzwerk bieten unsere zielführenden Workflows eine umfassende Lösung für die Besetzung und das Casting eurer Projekte.

We have been working hand in hand with productions from all over Europe since 2010. We processed over 85.000 applications for this purpose. Our modeling agency displays your product and brand communication via a curated file. We want to accompany you holistically and offer you talent for the present and the future. We fill your projects in the flow through castings throughout Germany and a supra-regional pool.

Together we will find models who ideally represent your brand within your budget. We ensure that your models are available for your shoots and, once approved, we will book them. You can concentrate on the essentials while we take care of all legal issues relating to licenses, buy-outs and more. We take care of briefings and logistical processing and are always available to deal with individual concerns so that your project is a perfect fit.

Customer proven

We are happy to accompany you in the long term, because our view extends far beyond individual services. Our goal is to be a reliable partner in your art buying process by constantly facing new challenges - with innovation and proactive action. We remain true to our values ​​and offer you stability for your bookings and our mutual success.

Flexible model booking

Regardless of whether it is a commercial objective or to expand your portfolio, we are your agency in this matter and offer you free and non-binding services from pre-selection to obtaining binding booking options.

• Individually tailored offer creation
• Project-related pre-selections and castings
• Non-binding option inquiries

Our models for your projects

Gabor: style and comfort combined

Bluphoria: wellness and well-being

We take care

Do you have any questions? No problem! Our booking team in Cologne will be happy to answer you quickly and reliably. Find out more and find out more about our projects and services or get advice. Whether you would like to get in touch or make a project inquiry – we look forward to hearing from you!

Your selection

Would you like to start a project with us or do you have a question?

• Wiener Models
• South Africa
• Creators by Kult
• Kult Artists

• Development
• Sustainable
• Fitness/sport
• families & couples
• Makeup Artists & Stylists
• Hands, legs & feet
• families & Couples
• favourites 0

Our agency represents a variety of professional models, actors and talent throughout the UK and Europe

Base Models is one of the few genuinely established UK commercial modelling agencies. We are London based and represent a variety of Models, Artist’s & Content Creator’s. We work with a large variety of clients, covering all area’s within the industry throughout the UK and Europe. With continued industry vision we see the opportunities for new, exciting talent and strive to develop tomorrows next top models and artists.

Influencers

Our Clients

Our ever growing client base hosts some of the world’s leading brands. With over thirty years industry experience, Base is at the forefront of the Commercial Modelling & Influencer industry.

Our Services

Our high-end talent and models are hired across the creative markets; including national and international advertising campaigns in print, digital and broadcast media. Since forming in 1982, we have enjoyed providing models for the largest global communications organisations, advertising agencies and clothing brands. Understanding client’s requirements and our deep knowledge of the modelling industry, enables us to provide a fast, professional service, specifically tailored to production and casting briefs.

Base Newsletter

Receive updates direct to your inbox on all things model and fashion related, including exclusive insights to London's hottest events and shows.

• Apply to join
• terms & conditions
• Mediaslide model agency software
• © Copyright 2019 Base Models
• BOURNEMOUTH
• SOUTHAMPTON

• Application

BECOME A MODEL

A dream job, really! Nationally for e-commerce shoots, internationally on the catwalk as a model.

Model agency and management

CM Models – Your model agency and model management! We search and scout (discover) models for our clients in fashion, media and marketing. We work closely with our clients from individual brands to photographers, advertising agencies and PR agencies and know their requirements and wishes. According to these criteria, we look for the best new models , curved models , male models and creators for our clients and brands! Our team works 100% for every booking. Do you have any questions?

• Customers: Contact
• Models: Application

Book models: Our job

For clients, we enable carefree processes through good cooperation, from casting and sedcard selection to final travel management and processing. You can focus entirely on your production – with models on time, on set.

For models, we offer as management the right paths and steps you need to take to work successfully as a model. Our team brings over 20 years of experience to all bookings. Our clients appreciate this and it shows in our references .

Still have questions? Here are all the answers and your contacts.

Inquiries & Contact

We look forward to your inquiry!

• CM Models Agency and Management
• Models for advertising: photo and video production
• Models for fashion: Fitting, showroom, fashion show
• International Model Management (abroad)
• Rights of use, travel management, etc.
• Model Scouting (discover)
• Our contact persons: Contact

CM for customers & brands

Our tasks as a model agency for clients and brands:

After the first email, the first contact, our model bookers check all the important criteria. This includes, for example, the model’s look, the tasks on location, availability on the production day, travel planning. You will receive a personal selection of models from us with photo material, video material and Polaroids (natural photos in daylight).

Fashion shows, photo shoots for e-commerce , social media , fashion shows , advertising campaigns – all you need! As soon as we receive your booking request, we will make a personal selection of models for you and send you the sedcard selection. Your advantage: Focus on your tasks, thanks to professional models on location with charisma, objectives and smooth implementation on schedule.

• About us: Model agency

CM for models

What does our CM Models Management do for you?

We build up our models (New Faces ) step by step. Often at the age of 15 , 16 , during their school years and later as models abroad, at the age of 18, 19, at the big fashion weeks . In collaboration with international partners and model agencies in Milan , Paris , London , Tokyo , New York and many other metropolises. Step by step. So that your modeling career is well planned and you have the greatest possible success for yourself.

• Learn: Become a model

Videos, backstage, photos and news:

Further selected customers and references of CM.

Now at CM: Adam from Poland

Korean skincare: amie shines in yepoda beauty shoot, jimmy choo, michael kors, versace and kate spade – now under one roof, philipp plein milan fashion week fw24/25 show x diego pooth.

Want to discover more? Click here for our news

Book a model

How do we support our clients? As a modeling agency , we advise, for example, in the pre-selection of models and provide models for your fashion show, photo shoot in e-commerce, social media content, POS campaigns, advertising films – all you need!

We look forward to your project!

Personal model selection & advice

Our work begins long before the booking. We sift through thousands of model applications throughout the year. In addition, there is proactive scouting to discover talents who would not have expected to have the right qualifications. This is followed by the first appointments, the casting at the agency, the first photo shoots for the portfolio and experiences – all in preparation for your bookings!

As soon as we receive your booking request, we select your personal selection of models with the right requirements for your ideas. Depending on the client, with a very different focus: the look, the size, the clothing, available dates, location in Europe, America or Asia. This is followed by travel management, depending on the job, all from the background – so you can concentrate fully on your project.

• Model agency

Models for your photo shoot

E-commerce, lookbooks, POS campaigns – new products have to be produced for many sales and marketing activities. Photos for your own online store, photos for retail, lookbooks for customers or even online, PR and POS campaigns. With us you will find strong models for your next production in the photo studio.

• Social Media

Models for your commercial

Social media content, commercials, television – moving images, whether commercials or small social content, require even more skill than photos. Another important aspect during applications and castings. With us, you can book models with the right charisma without any worries!

• Advertising campaigns

Models for your fashion show

Fitting, showroom, fashion show – the presentation of fashion, new collections and lines is one of the basics of every model. We attach great importance to our models gaining experience on the catwalk at a young age, also through training in posture and choreography. Convince your customers with models from CM.

• Fashion show

Fashion show, social media, e-commerce, campaigns

Here are a few examples from CM YouTube . Here you can find more references .

How do you book a model?

For the model booking you ideally already have 1) exact ideas of the model (look, age, etc.) and 2) all important data for the booking (date, location, use, etc.). This is the quickest way for us to send you a sedcard selection for your project!

• Model description
• Information about the model casting / job

Model description – There are very different factors for different jobs. Body size for the catwalk, skin for beauty jobs, the right age for the target group of the campaign, hair color and much more. Always mention a few key points so that we know what you have in mind.

Information about the model casting / job – Ideally, this includes: production date, location, start and end time, the job itself (fitting, fashion show, photo shoot, commercial, etc.), as well as the subsequent use and utilization of the production (media, time and territory).

The more complete the briefing, the better!

Contact us Customers

Models Curved New Faces Men Models Influencer

E-Commerce Social Media Fashion show Advertising campaigns

• Become a model

What does model management do?

We build up our models (New Faces) step by step. Often at the age of 15 or 16, during their school years and later abroad. At the age of 18 or 19, they then go to the big fashion weeks. In cooperation with international partners and model agencies in Milan, Paris, London, Tokyo, New York and many other major cities.

We start with tips, communicate with your parents, give short coaching and training sessions, all for you. We organize the first photo shoots with good photographers, send you your first castings and jobs. Everything step by step. So that your modeling career is well planned and you have the greatest possible success for yourself.

Whether interviews or coaching sessions, we want our models to develop extremely well.

After that: Modeling abroad! Paris, Milan, London, New York.

Step by step! Modeling

Here is a brief overview.

Requirement – The right dimensions, the optimum weight, the perfect look – there is no such thing. Every brand has its own target group. Parisian fashion brands tend to focus on thin models, in Germany more and more curvy models are being booked and in general: diversity. No matter what your look is like, your first model application is quick and costs nothing. If you want to become a model, give it a try and apply!

Here are a few more tips:

• Becoming a model at 14
• Becoming a model at 15
• Becoming a model at 16

Application and photos

Application – Polaroids (photos) and the first casting in our model agency are the 2 central steps. Polaroids are simple, completely natural photos of you in daylight. No make-up, no styling, just you, completely natural. Preferably a portrait and a full-body photo. Add a few contact details and measurements and you’re done! That’s the quickest way to a modeling contract.

You want to apply? Here we go:

• Model application @ CM

The first castings and jobs

Becoming a model – Now it’s all about your model portfolio (photos) and your personal development, with your first shoots with good photographers and your first small job. Are you still at school? Then school has absolute priority! Modeling really gets going after you leave school.

International – With our model management you can not only work here in Germany, but also with our local partner agencies throughout Europe (Paris , Milan and London ), as well as internationally in cities such as New York , Shanghai or Tokyo .

▷ CM X Women

▷ CM X Curved

We use cookies 🍪 ok for you?

Cookie and Privacy Settings

We may request cookies to be set on your device. We use cookies to let us know when you visit our websites, how you interact with us, to enrich your user experience, and to customize your relationship with our website.

Click on the different category headings to find out more. You can also change some of your preferences. Note that blocking some types of cookies may impact your experience on our websites and the services we are able to offer.

These cookies are strictly necessary to provide you with services available through our website and to use some of its features.

Because these cookies are strictly necessary to deliver the website, refusing them will have impact how our site functions. You always can block or delete cookies by changing your browser settings and force blocking all cookies on this website. But this will always prompt you to accept/refuse cookies when revisiting our site.

We fully respect if you want to refuse cookies but to avoid asking you again and again kindly allow us to store a cookie for that. You are free to opt out any time or opt in for other cookies to get a better experience. If you refuse cookies we will remove all set cookies in our domain.

We provide you with a list of stored cookies on your computer in our domain so you can check what we stored. Due to security reasons we are not able to show or modify cookies from other domains. You can check these in your browser security settings.

These cookies collect information that is used either in aggregate form to help us understand how our website is being used or how effective our marketing campaigns are, or to help us customize our website and application for you in order to enhance your experience.

If you do not want that we track your visit to our site you can disable tracking in your browser here:

We also use different external services like Google Webfonts, Google Maps, and external Video providers. Since these providers may collect personal data like your IP address we allow you to block them here. Please be aware that this might heavily reduce the functionality and appearance of our site. Changes will take effect once you reload the page.

Google Webfont Settings:

Google Map Settings:

Google reCaptcha Settings:

Vimeo and Youtube video embeds:

The following cookies are also needed - You can choose if you want to allow them:

You can read about our cookies and privacy settings in detail on our Privacy Policy Page.

Address: Östra Hamngatan 50B 411 09 Gothenburg,  Sweden

Office Hours: Monday - Thursday 9-17

Friday 9-16

Lunch 12-13

Phone: +46 31 774 15 77

Email: [email protected] Instagram: @avenuemodellerse

• TWO CELEBRITY

WE ONLY USE @TWOMANAGEMENT.COM

NOT @TWOMANAGEMENTLA.COM

IN DOUBT CONTACT US

• LOS ANGELES
• SCANDINAVIA

Los Angeles

development

Paloma Elsesser x Marni Jam 2024

Ahmed Richards | Tom Ford Mens F/W 2024

Sihana | Acne Paper Summer 2024

Georgia Palmer | Vogue Spain July 2024

Alex Consani | W China June 2024

Kristen McMenamy | W June 2024

He Cong | W China June 2024

Mary Ukech | Harper's Bazaar June 2024

Hailey Bieber | Saint Laurent S/S 2024

Litay | Vautrait F/W 2024

Bella Hadid | Saint Laurent F/W 2024

Kristen McMenamy | Vivienne Westwood F/W 2024

Ludovic de Saint Sernin F/W 2024

Bibi Breslin | Epoch Summer 2024

Hari Nef | Dust Summer 2024

Ashley Graham | Vogue CS July 2024

Maty | H&M S/S 2024

George Barnett | Gucci Men's F/W 2024

Clement Chabernaud | Gucci Men's F/W 2024

Georgia Palmer | Sunday Times Style June 2024

Mary Ukech | Lanvin Resort 2025

Sherry Shi | Harper's Bazaar Singapore June 2024

Aweng Chuol | Mission S/S 2024

• Family & Friends
• Influencers
• Meet The Team

Inclusive Modeling Agency Europe

Championing disabled, visibly different, non-binary, and trans models.

Zebedee aims to change the way disability, visible difference, and gender identity are portrayed in fashion and wider media.

“Disability is often left out of the diversity debate; we often receive briefs looking for ‘diversity’, but with no mention of disability, alternative appearances, or trans/non-binary – and we want to change this. We want it to be the norm that REAL diverse media becomes commonplace.” - Laura Winson & Zoe Proctor, Founders

Zebedee was established by co-founders Laura and Zoe in 2017 with a passion for diversity. Today we are the world's leading inclusive talent agency, representing models and actors with disabilities, visible differences, non-binary identities, and transgender identities in the UK , Europe , USA and Australia , and Japan . We work with talent all across Europe, with central hubs located in Paris, France, Italy, Germany, Netherlands, and Spain. Our pool of European models, actors, and creatives is constantly expanding, giving you access to unique and showstopping talent so that you can create campaigns that break through the noise.

We Partner With Brands Wanting to Make a Difference

Big or small, our perfect partners are brands and casting directors who understand the importance of making their marketing campaigns and shows more inclusive and address the staggering underrepresentation in the advertising and media industry.

We are already working with some of the world’s most iconic brands – including Gucci, Burberry, Mercedes, Vogue, Estee Lauder, Disney, The BBC and HBO, and we’d love for you to join them on our collective journey towards more diverse casting.

There is still much to do, but with your help, we can continue to bring balance to the industry – one inclusive casting at a time.

Work With Europe’s Leading Inclusive Talent Agency

Our talent is different – and so are we..

Choosing Zebedee Talent means access to Europe's most diverse talent pool as well as a wide range of creative campaign resources. We believe in promoting community, confidence, and education, and our commitment to our models goes above and beyond the typical talent agent. 

As the leading inclusive talent agency in Europe, we regularly put on events aimed at developing both life and professional skills for our network, and we support our talent with the utmost compassion and understanding – something we expect from our clients too.

While we are conscious of the challenges facing our talent, we are also aware that this may be your first time working with our innovative models.

While some models may require a bit more attention and planning before a shoot, we will work with you to make sure that everything runs smoothly, offering webinars and resources to help you understand every aspect of disability, difference, and gender, so that you also feel as comfortable as our models feel in front of the camera.

Despite any reservations or preconceptions, working with diverse talent is an incredibly rewarding experience for everyone involved, and for the wider viewing public once your campaign is ultimately released.

DIVERSITY BEHIND THE CAMERA

We encourage our clients to consider diversity, both in front and behind the camera. Speak to us about our talented photographers, hair and make-up artists, videographers, stylists, producers, directors and more.

CONSULTANCY

Our consultancy team can help you ensure your spaces and projects are inclusive too – offering training, guest speakers, and workplace, culture and policy reviews.

We can also offer support during the creative process, checking the stories you tell are sensitive and authentic – plus our access coordinators can help during casting and shoots, ensuring everyone’s needs are properly catered for.

Want us to suggest talent instead?

We know a thing or two about finding the perfect talent to fit your needs. If you would like the team to help shortlist talent on your behalf - please send a short brief via our contact form, and we’ll help you find the perfect star for your campaign.

The European Model Showcase gives you the opportunity to meet agents from many of Europe’s top modelling agencies. Here are just some of the agencies we’ve hosted since 2005.

2MModel Milano

5th avenue model management barcelona, body & soul models hamburg, brave models milano, city models agency paris, crystal models paris, d m g models paris, elite world paris, esee models shanghai, exclusive mgmt paris, fleming international barcelona, ford models, inc. paris, francina models barcelona, gladys model mgmt paris, hype models paris, img models paris, karin models paris, leni’s model management london, mademoiselle paris, magteam models warsaw, marilyn agency paris, martine’s women agency paris, nathalie model agency paris, nevs london, new madison paris, next models paris, okay models hamburg, oui management paris, studio klrp paris, success paris, visage osaka, viva model management paris, vivienne model management munich, wilhelmina one asia bangkok, women mgmt paris, world top inc. tokyo, yoshie inc. tokyo.

This site uses cookies to provide web functionality and performance measurement.

ATM is a top model agency with its headquarter in Vienna and manages models and talents from all over the world.

We are a young team with a personal and caring attitude and booking national and international jobs with the biggest clients this industry has to offer.

Our persistency and unconventional management style built our good reputation over the last years and made ATM a very well known agency throughout the world of fashion and a top agency according to models.com.

Our main concern is to always provide our clients not just with the right face for their brand, but also with a professional model with the best attitude suited for their needs.

Get addicted like us, to the beauty, the great personalities of our models and to our work philosophy.

ATM is like a big family, where we take care of each other. #weareaddicted

– addiction –

The purest and most absolute obsession.

The heart starts to race. Adrenaline and dopamine rushing through the body, a whole moment, intoxicated by joy.

That’s the moment when you see the perfect model.

Become a Model

BECOME A MODEL

ADDICTED TO MODELS is always on the lookout for new faces from all over the world. If you want to become part of our family, just fill out the form below or email all the information and the required pictures to [email protected].

PHOTOGRAPHS

The pictures don‘t have to be professional. Please take care that you take them with natural bright light in front of a simple background (like a white wall). Also pay attention that your face is clearly visible (no hair in your face) and that you wear tight, simple clothes. We want to see your natural beauty, so don‘t wear make-up.

HEAD SHOT EXAMPLE

PROFILE SHOT EXAMPLE

3/4 PROFILE SHOT EXAMPLE

FULL BODY SHOT EXAMPLE

Welcome on board Maxim! A new addition to our Addicted Family! #newonboard#newface#newmodel#malemodel#malemodeling#malemodeltrending#modelagentur#modelagency#addictedtomodel

Alba for @lofficielarabia #lofficielarabia#lofficiel#editorialmodel#editorialmodels#editorialshoot#editorialphotography#magazinemodels#magazinemodel#modelagency#modelagentur

Jasmin for @brunobananiofficial #lingerielove#lingeriemodel#lingeriephotography#brunobananilingerie#fashionmodel#commercialmodels#commercialmodeling#campaignphotoshoot#modelagency#modelagentur

Casting vs photos 📸 Meet Kate! #femalemodel#femalemodeling#castingvsphotos#addictedtomodels#modelagency#modelagentur#modelcastingcall#modelcasting#modelswanted

Sarah for @mercedesbenz Photographer: @ppppppppppppaesn Styling: @tommytrvn_ Retouch: @nicolarehbein @julianbgr #mercedesbenz#mercedes#campaignshoot#commercialshot#commercialmodels#commercialmodeling#modelswanted#modelagentur

We are happy to announce we are now representing Masho!📸 #newonboard#newface#femalemodels#femalemodeling#modelswanted#modelscouting#modelsearch#modeling#modelagentur#modelagency

ADDICTED TO MODELS

Koppstraße 38/21

1160 Vienna, Austria

+43677 614 386 66

[email protected]

MODEL APPLICATIONS ONLY VIA EMAIL. NO OFFICE VISITS OR PHONE CALLS.

• Apply as a model
• Register as a customer
• Model search

Prestige Modelmanagement is looking for part-time and full-time model scouts

THE INTERNATIONAL ONLINE MODEL AGENCY

Models like you and me the leading portal for models and the promotional faces, 50-plus models, babies and children as well as actors and extras from 0 to 80..

YOU'RE IN THE RIGHT PLACE!

Do you want to become a model?

Prestige Modelmanagement is a global online model agency with European headquarters in VIENNA as well as offices in many other countries. We offer you the opportunity to fulfil your dream of modelling, and give you and/or your child the chance to introduce yourself online to reputable clients worldwide , and so be discovered.

APPLICATION IS FREE OF CHARGE AND ABSOLUTELY NON-BINDING.

WE WANT YOU!

For brochures/catalogue/fashion photos, fashion shows and advertisements in the whole of Austria, Germany and Switzerland and many other countries in Europe and worldwide. Are you aged between 0 and 80 , tall or short, slim or plump, young or young at heart, attractive, or distinctive-looking? Advertising needs YOU! In principle, (almost) anyone with great charisma, self-confidence and a well-groomed and appealing appearance can join the fashion and advertising business and become a model!

HOW DO I APPLY FOR MYSELF OR MY CHILD?

Becoming a model is easy.

Choose the right category so that you are directed to the right portal. Then click on the 'apply as a model' button. This will take you to an application form where you will be asked to enter your e-mail address and your personal details, and upload a good photo. A team of experts will then review your details. Within a few days, you will receive an automatically-generated customer number and a request to call us.

The PRESTIGE experts' tip

The more recognisable you or your child are on the photos, the easier it is for our Casting Team to assess your online application. Always ensure you or your child appear alone on the photo.

FROM OUR MODELS' OWN MOUTHS

Patrick, 55, "I applied to Prestige Modelmanagement because I wanted more variety in my life. I got that by modelling!"

Tim, 12 "The girls at school laughed at first, but once they'd seen me in a fashion brochure, they were proud to be in my class!"

Alexandra, 25, "I wanted to do something I could enjoy alongside my job, and something that would bring me a regular extra income. I achieved that with Prestige Modelmanagement "  

Katharina, 1, and Giuliana, 8 months, "We had only been on the agency's books for two weeks when we were booked for Billa. We would like to thank Prestige Modelmanagement for their professional support"

As customer

INFORMATION FOR CLIENTS

Search, find, and book online immediately.

Prestige Modelmanagement supports you as a client in quickly and cost-effectively finding the right people for your projects. We offer a wide range of different models, promotional faces and character types for all your various projects. Whether you're an advertising agency or editor looking for the right model, a photographer seeking people for a professional photo shoot, or a TV production company needing particular candidates/extras/actors etc. - we're here to help you in your search!

We see ourselves as a full-service agency, offering both placement and casting services. Whatever your query - just give us a call! As a client (photographer - advertising agency - film production company, etc...), you can outsource your jobs and casting requirements via our agency at no cost, and complete your model bookings.

We offer qualified model coaching for every assignment and job. Prestige Modelmanagement's services are defined by interesting collaborations and partnerships with make-up artists, photographers and stylists.

As a client, you have direct access to our online database, and can book models online.

There are no incidental costs for clients and customers.

COMPANY MANAGEMENT COMMENTS

People always think they're too fat, too thin, too short, too unattractive, too old or whatever else to work as a photo model or promotional face. But advertising has now discovered 'real people' like you and me. It doesn't matter to us whether you have perfect model measurements, or inner beauty. Whatever your clothing or body size. Just go for it! You may be just what the world of fashion and advertising is looking for?

Our models' profiles and booking cards are not publicly available. Prestige Modelmanagement will make your photos or the photos of your child available only to selected agencies, who receive a login code only when we have assessed them. Access to all online profiles/booking cards requires a login (e-mail & password) because we take the data security of the models we place very seriously. The client can then select according to criteria such as age, hair and eye colour, size etc.

SUCCESSFUL TOGETHER!

Prestige Modelmanagement will set up a personal user account for you where you can create a personal profile for you and/or your child, including a booking card that couldn't be easier to manage. Here, you can upload up to ten current photos (portraits and full-length shots) of you and/or your child, and enter your personal details. We treat all this information in complete confidence. Customers then see only information about your age, gender, size, clothing size etc.

Prestige Modelmanagement acts as a broker between clients and yourself. We will tell you about assignments by telephone or e-mail, and you can of course turn an offer down at any time.

WE LOOK FORWARD TO HEARING FROM YOU!

MODEL/CUSTOMER LOGIN

SVEND TOFTE BJØRN | BERLUTI

LUKE FARNWORTH for GUY LAROCHE AW23 CAMPAIGN

ALEXANDER GUDMUNDSSON for THE ARTELIER & VICTOR VON SCHWARZ 080 BARCELONA FASHION WEEK

SVEND TOFTE BJØRN for ADER ERROR x MAISON KITSUNÉ

ALEXANDER GUDMUNDSSON for RAINS SS21

DIMA DIONESOV for GQ STYLE Russia

SVEND TOFTE BJØRN for RAINS SS21 Drifter Campaign

LUKE FARNWORTH for BOGLIOLI FW20 Campaign

Interview: A Split Second with PAVEL NIRSHA

Interview: A Split Second with VALENTIN SKRYPNIKOV

LUKE FARNWORTH for DRUMOHR FW20

ALEXANDER GUDMUNDSSON for MONCLER 1952 FW20 eComm

DIMA DIONESOV portrait series by ARTEM POMENCHUK

Alexander Gudmundsson for FW2021 Paris

FENDI A/W 2021

MONCLER 1952 F/W 2020

ENFANTS RICHES DÉPRIMÉS F/W 2020

DUNHILL F/W 2020

CRAIG GREEN F/W 2020

LI NING F/W 2020

SACAI F/W 2020

40 Facts About Elektrostal

Written by Lanette Mayes

Modified & Updated: 01 Jun 2024

Reviewed by Jessica Corbett

Elektrostal is a vibrant city located in the Moscow Oblast region of Russia. With a rich history, stunning architecture, and a thriving community, Elektrostal is a city that has much to offer. Whether you are a history buff, nature enthusiast, or simply curious about different cultures, Elektrostal is sure to captivate you.

This article will provide you with 40 fascinating facts about Elektrostal, giving you a better understanding of why this city is worth exploring. From its origins as an industrial hub to its modern-day charm, we will delve into the various aspects that make Elektrostal a unique and must-visit destination.

So, join us as we uncover the hidden treasures of Elektrostal and discover what makes this city a true gem in the heart of Russia.

Key Takeaways:

• Elektrostal, known as the “Motor City of Russia,” is a vibrant and growing city with a rich industrial history, offering diverse cultural experiences and a strong commitment to environmental sustainability.
• With its convenient location near Moscow, Elektrostal provides a picturesque landscape, vibrant nightlife, and a range of recreational activities, making it an ideal destination for residents and visitors alike.

Known as the “Motor City of Russia.”

Elektrostal, a city located in the Moscow Oblast region of Russia, earned the nickname “Motor City” due to its significant involvement in the automotive industry.

Home to the Elektrostal Metallurgical Plant.

Elektrostal is renowned for its metallurgical plant, which has been producing high-quality steel and alloys since its establishment in 1916.

Boasts a rich industrial heritage.

Elektrostal has a long history of industrial development, contributing to the growth and progress of the region.

Founded in 1916.

The city of Elektrostal was founded in 1916 as a result of the construction of the Elektrostal Metallurgical Plant.

Located approximately 50 kilometers east of Moscow.

Elektrostal is situated in close proximity to the Russian capital, making it easily accessible for both residents and visitors.

Known for its vibrant cultural scene.

Elektrostal is home to several cultural institutions, including museums, theaters, and art galleries that showcase the city’s rich artistic heritage.

A popular destination for nature lovers.

Surrounded by picturesque landscapes and forests, Elektrostal offers ample opportunities for outdoor activities such as hiking, camping, and birdwatching.

Hosts the annual Elektrostal City Day celebrations.

Every year, Elektrostal organizes festive events and activities to celebrate its founding, bringing together residents and visitors in a spirit of unity and joy.

Has a population of approximately 160,000 people.

Elektrostal is home to a diverse and vibrant community of around 160,000 residents, contributing to its dynamic atmosphere.

Boasts excellent education facilities.

The city is known for its well-established educational institutions, providing quality education to students of all ages.

A center for scientific research and innovation.

Elektrostal serves as an important hub for scientific research, particularly in the fields of metallurgy , materials science, and engineering.

Surrounded by picturesque lakes.

The city is blessed with numerous beautiful lakes , offering scenic views and recreational opportunities for locals and visitors alike.

Well-connected transportation system.

Elektrostal benefits from an efficient transportation network, including highways, railways, and public transportation options, ensuring convenient travel within and beyond the city.

Famous for its traditional Russian cuisine.

Food enthusiasts can indulge in authentic Russian dishes at numerous restaurants and cafes scattered throughout Elektrostal.

Home to notable architectural landmarks.

Elektrostal boasts impressive architecture, including the Church of the Transfiguration of the Lord and the Elektrostal Palace of Culture.

Offers a wide range of recreational facilities.

Residents and visitors can enjoy various recreational activities, such as sports complexes, swimming pools, and fitness centers, enhancing the overall quality of life.

Provides a high standard of healthcare.

Elektrostal is equipped with modern medical facilities, ensuring residents have access to quality healthcare services.

Home to the Elektrostal History Museum.

The Elektrostal History Museum showcases the city’s fascinating past through exhibitions and displays.

A hub for sports enthusiasts.

Elektrostal is passionate about sports, with numerous stadiums, arenas, and sports clubs offering opportunities for athletes and spectators.

Celebrates diverse cultural festivals.

Throughout the year, Elektrostal hosts a variety of cultural festivals, celebrating different ethnicities, traditions, and art forms.

Electric power played a significant role in its early development.

Elektrostal owes its name and initial growth to the establishment of electric power stations and the utilization of electricity in the industrial sector.

Boasts a thriving economy.

The city’s strong industrial base, coupled with its strategic location near Moscow, has contributed to Elektrostal’s prosperous economic status.

Houses the Elektrostal Drama Theater.

The Elektrostal Drama Theater is a cultural centerpiece, attracting theater enthusiasts from far and wide.

Popular destination for winter sports.

Elektrostal’s proximity to ski resorts and winter sport facilities makes it a favorite destination for skiing, snowboarding, and other winter activities.

Promotes environmental sustainability.

Elektrostal prioritizes environmental protection and sustainability, implementing initiatives to reduce pollution and preserve natural resources.

Home to renowned educational institutions.

Elektrostal is known for its prestigious schools and universities, offering a wide range of academic programs to students.

Committed to cultural preservation.

The city values its cultural heritage and takes active steps to preserve and promote traditional customs, crafts, and arts.

Hosts an annual International Film Festival.

The Elektrostal International Film Festival attracts filmmakers and cinema enthusiasts from around the world, showcasing a diverse range of films.

Encourages entrepreneurship and innovation.

Elektrostal supports aspiring entrepreneurs and fosters a culture of innovation, providing opportunities for startups and business development .

Offers a range of housing options.

Elektrostal provides diverse housing options, including apartments, houses, and residential complexes, catering to different lifestyles and budgets.

Home to notable sports teams.

Elektrostal is proud of its sports legacy , with several successful sports teams competing at regional and national levels.

Boasts a vibrant nightlife scene.

Residents and visitors can enjoy a lively nightlife in Elektrostal, with numerous bars, clubs, and entertainment venues.

Promotes cultural exchange and international relations.

Elektrostal actively engages in international partnerships, cultural exchanges, and diplomatic collaborations to foster global connections.

Surrounded by beautiful nature reserves.

Nearby nature reserves, such as the Barybino Forest and Luchinskoye Lake, offer opportunities for nature enthusiasts to explore and appreciate the region’s biodiversity.

Commemorates historical events.

The city pays tribute to significant historical events through memorials, monuments, and exhibitions, ensuring the preservation of collective memory.

Promotes sports and youth development.

Elektrostal invests in sports infrastructure and programs to encourage youth participation, health, and physical fitness.

Hosts annual cultural and artistic festivals.

Throughout the year, Elektrostal celebrates its cultural diversity through festivals dedicated to music, dance, art, and theater.

Provides a picturesque landscape for photography enthusiasts.

The city’s scenic beauty, architectural landmarks, and natural surroundings make it a paradise for photographers.

Connects to Moscow via a direct train line.

The convenient train connection between Elektrostal and Moscow makes commuting between the two cities effortless.

A city with a bright future.

Elektrostal continues to grow and develop, aiming to become a model city in terms of infrastructure, sustainability, and quality of life for its residents.

In conclusion, Elektrostal is a fascinating city with a rich history and a vibrant present. From its origins as a center of steel production to its modern-day status as a hub for education and industry, Elektrostal has plenty to offer both residents and visitors. With its beautiful parks, cultural attractions, and proximity to Moscow, there is no shortage of things to see and do in this dynamic city. Whether you’re interested in exploring its historical landmarks, enjoying outdoor activities, or immersing yourself in the local culture, Elektrostal has something for everyone. So, next time you find yourself in the Moscow region, don’t miss the opportunity to discover the hidden gems of Elektrostal.

Q: What is the population of Elektrostal?

A: As of the latest data, the population of Elektrostal is approximately XXXX.

Q: How far is Elektrostal from Moscow?

A: Elektrostal is located approximately XX kilometers away from Moscow.

Q: Are there any famous landmarks in Elektrostal?

A: Yes, Elektrostal is home to several notable landmarks, including XXXX and XXXX.

Q: What industries are prominent in Elektrostal?

A: Elektrostal is known for its steel production industry and is also a center for engineering and manufacturing.

Q: Are there any universities or educational institutions in Elektrostal?

A: Yes, Elektrostal is home to XXXX University and several other educational institutions.

Q: What are some popular outdoor activities in Elektrostal?

A: Elektrostal offers several outdoor activities, such as hiking, cycling, and picnicking in its beautiful parks.

Q: Is Elektrostal well-connected in terms of transportation?

A: Yes, Elektrostal has good transportation links, including trains and buses, making it easily accessible from nearby cities.

Q: Are there any annual events or festivals in Elektrostal?

A: Yes, Elektrostal hosts various events and festivals throughout the year, including XXXX and XXXX.

Elektrostal's fascinating history, vibrant culture, and promising future make it a city worth exploring. For more captivating facts about cities around the world, discover the unique characteristics that define each city . Uncover the hidden gems of Moscow Oblast through our in-depth look at Kolomna. Lastly, dive into the rich industrial heritage of Teesside, a thriving industrial center with its own story to tell.

SME definition

Small and medium-sized enterprises (SMEs) represent 99% of all businesses in the EU. The definition of an SME is important for access to finance and EU support programmes targeted specifically at these enterprises.

What is an SME?

Small and medium-sized enterprises (SMEs) are defined in the EU recommendation 2003/361 .

The main factors determining whether an enterprise is an SME are

• staff headcount
• either turnover or balance sheet total

These ceilings apply to the figures for individual firms only. A firm that is part of a larger group may need to include staff headcount/turnover/balance sheet data from that group too.

Further details include

• The revised user guide to the SME definition (2020) (2 MB, available in all EU languages)
• Declaring your enterprise to be an SME (the form is available in all languages as an annex in the revised user guide)
• The SME self-assessment tool which you can use to determine whether your organisation qualifies as a small and medium-sized enterprise

What help can SMEs get?

There are 2 broad types of potential benefit for an enterprise if it meets the criteria

• eligibility for support under many EU business-support programmes targeted specifically at SMEs: research funding, competitiveness and innovation funding and similar national support programmes that could otherwise be banned as unfair government support ('state aid' – see block exemption regulation )
• fewer requirements or reduced fees for EU administrative compliance

Monitoring of the implementation of the SME definition

The Commission monitors the implementation of the SME definition and reviews it in irregular intervals. Pursuant to the latest evaluation, the Commission concluded that there is no need for a revision.

On 25 October 2021, we informed stakeholders by holding a webinar with presentations on the SME evaluation's results and next steps.

Supporting documents

• Study to map, measure and portray the EU mid-cap landscape (2022)
• Staff working document on the evaluation of the SME definition  (2021)
• Executive summary on the evaluation of the SME definition  (2021)
• Q&A on the evaluation of the SME definition  (2021)
• Final report on evaluation of the SME definition  (2018) (10 MB)
• Final report on evaluation of the SME definition (2012)  (1.8 MB)
• Executive summary on evaluation of the SME definition (2012)  (345 kB)
• Implementing the SME definition (2009)  (50 kB)
• Implementing the SME definition (2006)  (40 kB)

Share this page

• SMP WEDDINGS
• SMP’S VENUE BLOG
• LITTLE BLACK BOOK BLOG
• LBB INDUSTRY BLOG
• DESTINATION
• NEW ENGLAND
• THE NORTHWEST
• THE MIDWEST
• THE SOUTHWEST
• THE SOUTHEAST
• THE MID-ATLANTIC
• THE TRI-STATE AREA

Russia Weddings

• Real Weddings
• Bridal Week
• Engagements & Proposals
• Seasonal Wedding Trends
• Bridal Beauty
• Wedding Fashion Trends
• Vendor Guide
• DIY Projects
• Registry Guide
• Engagements & Proposals
• by Melissa Hammam
• comments ( )

Hands up if you’re ready to be dazzled! From a ceremony structure designed to float on water to a jaw-dropping reception room with flowers blooming from every service, we’re swooning over every bit of this wedding. If you can believe it, that’s just the beginning. Julia Kaptelova artfully shot every detail, like the ballet performance guests were treated to and snow falling from the ceiling for the first dance! Prepare to be amazed and take a visit to the full gallery .

From About You Decor … Our design is a symbol of dawn and a distant endless horizon. Ahead is a long, happy life without any borders. An international couple, Pavel and Cherry, met in London and have been walking together for many years.

From the Bride, Cherry… My husband and I we decided to have our summer wedding in Moscow because the city is where his roots are. As we knew we were going to have the other wedding ceremony in China, we wanted our Moscow one to be very personal and intimate. We’ve known each other since we were fourteen, together with many of our friends whom we’ve also known for a decade.

I didn’t want to walk down the aisle twice so the plausibility of my request quickly came into discussion. The open pontoon stage was constructed in order to facilitate the bridal entrance on water, although there were concerns about safety as the last thing we wanted was probably a drowned bride before she could get on stage, picture that! I have to say on that day it wasn’t easy to get on the pontoon stage from the boat, in my long gown and high heels. Luckily my bridesmaids still noticed even though they stood the furthest from me on the stage, and helped me out without prior rehearsal. My girls could just tell whenever I needed a hand or maybe they were just so used to my clumsiness. Who knows 😂

We all love our photographer Julia! She’s so talented and her style is so unique. Our beloved host Alex is exceptional who made everyone laugh and cry. It was truly a blessing to have so many kind and beautiful souls on our big day. Thank you all!

[iframe https://player.vimeo.com/video/384992271 600 338]

Photography: Julia Kaptelova Photography | Wedding Planner: Caramel | Cake: Any Cake | Invitations: Inviteria | Rings: Harry Winston | Band: Menhouzen | Grooms attire: Ermenegildo Zegna | Wedding Venue: Elizaveta Panichkina | Bridesmaids’ dresses: Marchesa | Bridesmaids’ dresses: Alice McCall | Bride’s gown : Jaton Couture | Bride’s shoes: Manolo Blahnik | Decor : About you decor | Earrings: Damiani | Muah: Khvanaco Studio | Video: Artem Korchagin

More Princess-Worthy Ballgowns

I’m still not convinced this Moscow wedding, captured to perfection by  Sonya Khegay , isn’t actually an inspiration session—it’s just  that breathtaking. From the beautiful Bride’s gorgeous lace wedding dress and flawless hair and makeup to the pretty pastel color palette and stunning ceremony and reception spaces, this wedding is almost too good to be true. Do yourself a favor and see it all in The Vault now!

From Sonya Khegay … It was the last day of April and still very cold in the morning. The weather forecast wasn’t pleasing and no one expected that the sun would come out, but miracles happen and light rain gave way to the warm rays.

I love how all the details went together, you could feel the harmony in everything throughout the entire wedding day from the morning until the fireworks.

A gentle look of the bride, elegant but so airy and unique decor, the fresh and light atmosphere of early spring and, of course, true happiness in the eyes. My heart becomes so warm from these memories, it is always a pleasure to see the birth of a new family of two loving hearts.

Photography: Sonya Khegay | Event Design: Latte Decor | Event Planning: Ajur Wedding | Floral Design: Blush Petals | Wedding Dress: La Sposa | Stationery: Special Invite | Bride's Shoes: Gianvito Rossi | Hair + Makeup: Natalie Yastrebova | Venue: Rodniki Hotel

• by Elizabeth Greene

You really can’t go wrong with simple: a beautiful Bride , perfectly pretty petals , loved ones all around. But add in an amazing firework show  to cap off the night and simple just became downright extraordinary. Captured by Lena Elisseva , with assistance by  Katya Butenko , this rustic Russian celebration is simply fantastic. See it all in the Vault right here !

From Lena Eliseeva Photo …  This cozy and warm summer wedding of gorgeous Natalia and Anton was in the middle of June. The young couple decided to organize their wedding themselves, and the day was very personal and touching. I am absolutely in love with rustic outdoor weddings, and this one is my favourite because of the free and easy atmosphere.

All the decor excluding the bride’s bouquet was made by a team of ten friends of the bride and groom. And it was charming – a light and beautiful arch, eco-style polygraphy and succulents, candy-bar with caramel apples and berries – sweet joys of summer.

At the end of ceremony the guests tossed up white handkerchiefs embroidered by Natalia’s own hands.

The most touching moment was the happy eyes of the groom’s grandmother, the most estimable person on the wedding. And the fireworks were a bright end to that beautiful day.

Photography: LENA ELISEEVA PHOTO | Floral Design: Katerina Kazakova | Hair And Makeup: Svetlana Fischeva | Photography - Assistance: Katya Butenko

These photos from Lena Kozhina are so stunningly beautiful – as in you can’t help but stop and stare – it’s hard to believe it’s real life. But these pics are proof of this gorgeous Bride and her handsome Groom’s celebration at Moscow’s Fox Lodge , surrounded by vibrant colors and breathtaking blooms . Oh, and the idea of prepping for your Big Day outside in the sun ? Brilliant. See more bright ideas right here !

From Lena Kozhina … When we met with the couple for the first time, we immediately paid attention to Dima’s behavior towards Julia. There was a feeling of tenderness and awe, and we immediately wanted to recreate this atmosphere of love, care and warmth on their Big Day.

Later, when we had chosen a green meadow and an uncovered pavilion overlooking a lake as the project site, it only highlighted a light summer mood with colorful florals and a great number of natural woods. The name of the site is Fox Lodge and peach-orange color, as one of the Bride’s favorites, set the tone for the whole design – from the invitations, in which we used images of fox cubs to elements of serving guest tables and other decorative elements with the corresponding bright accents.

Photography: Lena Kozhina | Event Planning: Ajur Wedding | Wedding Dress: Rosa Clara | Shoes: Marc Jacobs | Catering: Fox Lodge | Makeup Artist: Elena Otrembskaya | Wedding Venue: Fox Lodge | Cake and Desserts: Yumbaker | Decor: Latte Decor

From Our Partners

Thank you for visiting nature.com. You are using a browser version with limited support for CSS. To obtain the best experience, we recommend you use a more up to date browser (or turn off compatibility mode in Internet Explorer). In the meantime, to ensure continued support, we are displaying the site without styles and JavaScript.

• View all journals
• Explore content
• About the journal
• Publish with us
• Sign up for alerts
• Open access
• Published: 10 June 2024

Evidence for transient morning water frost deposits on the Tharsis volcanoes of Mars

• A. Valantinas   ORCID: orcid.org/0000-0001-9995-3335 1 , 2 ,
• N. Thomas 1 ,
• A. Pommerol   ORCID: orcid.org/0000-0002-9165-9243 1 ,
• O. Karatekin 3 ,
• L. Ruiz Lozano   ORCID: orcid.org/0000-0002-8084-5438 3 ,
• C. B. Senel   ORCID: orcid.org/0000-0002-7677-9597 3 , 4 ,
• O. Temel 3 , 5 ,
• E. Hauber   ORCID: orcid.org/0000-0002-1375-304X 6 ,
• D. Tirsch   ORCID: orcid.org/0000-0001-5905-5426 6 ,
• V. T. Bickel   ORCID: orcid.org/0000-0002-7914-2516 7 ,
• G. Munaretto 8 ,
• M. Pajola   ORCID: orcid.org/0000-0002-3144-1277 8 ,
• F. Oliva   ORCID: orcid.org/0000-0002-6271-3722 9 ,
• F. Schmidt   ORCID: orcid.org/0000-0002-2857-6621 10 , 11 ,
• I. Thomas   ORCID: orcid.org/0000-0003-3887-6668 12 ,
• A. S. McEwen 13 ,
• M. Almeida 1 ,
• M. Read 1 ,
• V. G. Rangarajan   ORCID: orcid.org/0000-0003-3694-7696 14 ,
• M. R. El-Maarry   ORCID: orcid.org/0000-0002-8262-0320 15 ,
• F. G. Carrozzo 9 ,
• E. D’Aversa   ORCID: orcid.org/0000-0002-5842-5867 9 ,
• F. Daerden   ORCID: orcid.org/0000-0001-7433-1839 12 ,
• B. Ristic 12 ,
• M. R. Patel   ORCID: orcid.org/0000-0002-8223-3566 16 ,
• G. Bellucci   ORCID: orcid.org/0000-0003-0867-8679 9 ,
• J. J. Lopez-Moreno   ORCID: orcid.org/0000-0002-7946-2624 17 ,
• A. C. Vandaele   ORCID: orcid.org/0000-0001-8940-9301 12 &
• G. Cremonese 8  

Nature Geoscience ( 2024 ) Cite this article

17k Accesses

2399 Altmetric

Metrics details

• Atmospheric dynamics
• Climate sciences
• Cryospheric science
• Geomorphology
• Inner planets

The present-day water cycle on Mars has implications for habitability and future human exploration. Water ice clouds and water vapour have been detected above the Tharsis volcanic province, suggesting the active exchange of water between regolith and atmosphere. Here we report observational evidence for extensive transient morning frost deposits on the calderas of the Tharsis volcanoes (Olympus, Arsia and Ascraeus Montes, and Ceraunius Tholus) using high-resolution colour images from the Colour and Stereo Surface Imaging System on board the European Space Agency’s Trace Gas Orbiter. The transient bluish deposits appear on the caldera floor and rim in the morning during the colder Martian seasons but are not present by afternoon. The presence of water frost is supported by spectral observations, as well as independent imagery from the European Space Agency’s Mars Express orbiter. Climate model simulations further suggest that early-morning surface temperatures at the high altitudes of the volcano calderas are sufficiently low to support the daily condensation of water—but not CO 2 —frost. Given the unlikely seasonal nature of volcanic outgassing, we suggest the observed frost is atmospheric in origin, implying the role of microclimate in local frost formation and a contribution to the broader Mars water cycle.

Similar content being viewed by others

Continuous sterane and phytane δ13C record reveals a substantial pCO2 decline since the mid-Miocene

Tipping point in ice-sheet grounding-zone melting due to ocean water intrusion

Proof of concept for a new sensor to monitor marine litter from space

The Tharsis Rise is a large volcanic province in the tropics of Mars 1 (latitude range: ±40° N, longitude range: 220–300° E). It is a broad topographic dome that rises about 5 km above the surrounding terrain and covers a region 5,000 km wide 2 . It contains some of the Solar System’s largest and tallest volcanoes 3 , such as Olympus Mons (21 km altitude), Arsia Mons (18 km), Ascraeus Mons (18 km) and Pavonis Mons (14 km), but also smaller shield volcanoes such as Ceraunius Tholus (9 km). Volcanic activity on Mars has been concentrated predominantly in this region throughout the planet’s geological history, persisting into current times, as evidenced by lava flows that are as recent as 2.4 million years old 4 . No current volcanic activity has been detected in Tharsis, although recent geophysical data show that Mars is still geodynamically active 5 , 6 , 7 .

Notable orographic water ice clouds and other atmospheric phenomena have been observed in Tharsis 8 , 9 , 10 , 11 , 12 . Water ice clouds play a fundamental role in cycling water on Mars, moving moisture for thousands of kilometres from polar regions to relatively dry equatorial areas 13 , 14 . In addition, Tharsis is situated along the route of an important cross-equatorial exchange of water vapour, where approximately 10 12  kg of water is annually transferred between the northern and southern hemispheres through the solstitial Hadley cells 15 . Atmospheric observations 16 have revealed a localized enrichment in water vapour above the Tharsis volcanoes, suggesting that an active exchange of water vapour between the regolith and the atmosphere may be ongoing, probably facilitated by desorption from the regolith and/or sublimation of frost. A subsequent study 17 confirmed the water-vapour enrichment over these areas but hypothesized that the local circulation pattern typical of the volcanic region is possibly responsible for the enrichment as it may carry considerable amounts of water vapour upslope.

Apart from the polar regions, water ice manifests on the surface as seasonal frost in mid- and low-latitude locations. NASA’s (the National Aeronautics and Space Administration’s) Viking 2 lander detected water frost at ~48° N 18 , 19 , 20 . In addition, orbital observations from a variety of instruments revealed that water frost can occur up to 13° S in the southern hemisphere and as low as 32° N on shaded pole-facing slopes 21 , 22 , 23 . However, the presence of frost at the tropics (~0° N latitude) was not expected because of higher average surface temperatures 24 and lower humidity 25 . Some studies predicted that on most of Mars’s surface, small amounts of H 2 O frost can condense nightly if radiative cooling is strong enough 26 , 27 . For example, extremely small amounts of water frost have been observed to condense near the equator on the high thermal emissivity calibration targets of NASA’s Opportunity rover 28 , 29 .

Most of the Martian atmosphere is composed of CO 2 gas, and therefore CO 2 frost can also form if surface temperatures are low enough 30 . On the basis of nightly surface temperatures and thermal modelling, it was shown that in the equatorial regions CO 2 frost may condense diurnally 29 , 30 , 31 , 32 . Predictions 30 , 31 indicated that putative CO 2 frost deposits may persist for only a few minutes after sunrise (~6:00 Local Solar Time ( lst )) before sublimating back into the atmosphere. Follow-up global surveys, utilizing early-morning colour observations from the Thermal Emission Imaging System (THEMIS 33 ) were conducted to search for these frosts in the equatorial regions, but no evidence of morning CO 2 frost was identified 34 .

Observations by the Colour and Stereo Surface Imaging System (CaSSIS 35 ) on board the European Space Agency’s (ESA’s) Trace Gas Orbiter (TGO) provide strong evidence for morning frost deposition on the equatorial Tharsis volcanoes. We present here these observations coupled with supporting evidence from other instruments and modelling.

Observations of frost

Early-morning images ( lst  = 7:11; latitude = 18.5° N, longitude = –133.5° E; spatial resolution = 4.5 m pixel –1 ) of Olympus Mons caldera acquired by CaSSIS (at utc 2022 November 25) in the late northern winter (solar longitude (Ls) ~345°) on Mars year (MY) 36 first revealed bluish deposits (at ~500 nm) on sections of the caldera floor and rim (Fig. 1 ). The CaSSIS observation suggests a spatial correlation between the bluish deposits and topography (Fig. 1d ). The deposits are concentrated on the caldera floor but are absent on well-illuminated warm slopes and farther north on the volcano flank. The finding was confirmed five days later with a High Resolution Stereo Camera (HRSC) 36 observation acquired on 2022 November 30 ( lst  = 7:20; latitude = 18.2° N, longitude = −133.2° E; spatial resolution = 800 m pixel –1 ), which revealed that the diffuse bluish ‘halo’ deposit was ubiquitous on the entire caldera floor and rim (Fig. 1b,c ). The halo is absent on the volcano flanks and is concentrated only at the mountain summit. During the CaSSIS detection, the Nadir and Occultation for Mars Discovery (NOMAD 37 ) spectrometer was operating and acquired a ride-along observation (instantaneous field of view = 17.5 km × 0.5 km). The nadir spectral data acquired in the NOMAD limb nadir and solar occultation (LNO) channel revealed that the deposit is frost (Fig. 1e ) as indicated by the elevated ice index values (more than 3 σ confidence; Methods and Supplementary Figs. 1 and 2 ).

a , Global view of Mars with white box marking the location of Olympus Mons. b , HRSC wide-angle image of Olympus Mons acquired in the early morning ( lst  = 7:20, Ls = 346.7°, latitude = 18.2° N, longitude = −133.2° E). The black dashed line indicates the orbit of the TGO corresponding to the images in d and e . The white box highlights the close up in c . c , Zoomed-in view of the Olympus Mons caldera. The white and blue dashed rectangles show the footprints of the CaSSIS and NOMAD-LNO observations, respectively. d , High-resolution (4.5 m pixel –1 ) CaSSIS colour image of frost on the caldera floor and northern rim of Olympus Mons ( lst  = 7:11, Ls = 344.1°). Frost is absent on the well-lit steep slopes. The blue rectangle marks the footprint of the one NOMAD-LNO observation that falls within the frost-covered area. e , NOMAD-LNO channel observation of the Olympus Mons caldera. The ice index values ( Methods ) indicate the presence of frost over the caldera floor (> µ  + 3 σ ). The coloured areas on the plot indicate the confidence intervals. HRSC image ID: hn889_0000 ( b , c ). CaSSIS colour image ID: MY36_022332_162_0_NPB ( d ). NOMAD-LNO observation ID: 20221125_082524 ( e ). Credit: b , ESA/DLR/FU Berlin; d , ESA/TGO/CaSSIS under a Creative Commons license CC-BY-SA 3.0 IGO .

Repeat imaging by HRSC shows that the frost deposits on top of Olympus Mons (Fig. 1b ) appear only in the early Martian morning ( lst  = ~7:00–7:30; latitude = 18.2° N, longitude = −133.2° E) and are spatially correlated with a geological bright halo unit (Extended Data Fig. 1a,d ). This unit may be dust that is relatively brighter than the surrounding material due to different grain size or texture 38 . This bright halo unit is also observed in Context Camera 39 images (Extended Data Fig. 2a ). Materials consisting of smaller particles may exhibit different thermophysical properties such as lower thermal conductivity 40 and high thermal emissivity 41 . Surfaces with such properties cool down more at night and warm up more slowly in the morning, further enhancing the likelihood and duration of frost formation. This latter point is illustrated by CaSSIS observations of frost on dust deposits that have not been removed by winds (Extended Data Fig. 2b,c ). As shown by CaSSIS, frost may also condense leeward of small craters where air-fall dust can accumulate and is perhaps less compact (Extended Data Fig. 2d ). Porous and less-compact materials provide more nucleation sites for frost formation 42 . Outside of the bright halo, frost is found near the northern rim of Olympus Mons, but its emplacement is more localized (Extended Data Fig. 2e–i ). In conclusion, the observed frost patterns on Olympus Mons, particularly in areas with geologically distinct bright dust deposits, underscore the importance of thermophysical properties such as low thermal conductivity and high thermal emissivity, as well as surface texture, in governing the formation, distribution and persistence of frost on Mars.

Within the CaSSIS database, 13 instances of frost have been found (Extended Data Fig. 3 ). These include detections not only on the largest Tharsis volcanoes of Olympus, Ascraeus and Arsia Montes but also on the smaller-sized Ceraunius Tholus shield volcano (Extended Data Fig. 4 ). In one case, the frost deposits on Arsia Mons (Fig. 2a ) are observed in the early Martian morning and during southern winter solstice ( lst  = ~8:00, Ls = ~90°, latitude = −8.7° N, longitude = −121.1° E). The frost line dividing warm and shadowed slopes is, however, not observed in the repeat CaSSIS observations of this location, which were acquired during late southern spring (Fig. 2b–d ). Photometric analysis shows that frost is associated with an increase in ratioed reflectance of up to 20% at wavelengths (Fig. 2e ; CaSSIS blue (BLU) filter bandwidth is 390–570 nm (ref. 43 )). The fact that frosty surfaces are sometimes brighter only at blue wavelengths, implying a lower spectral slope, can also be observed in a linearly stretched CaSSIS BLU filter image (Extended Data Fig. 5 and Methods ) and average spectra from a k -means clustering analysis 44 , 45 applied on a topographically corrected and photometrically normalized CaSSIS cube (Supplementary Fig. 3 ). The photometric and clustering analyses suggest that the frost deposits are probably very thin.

a , Frost on the shadowed slope of the crater in an early-morning observation during southern winter in MY 35 (latitude = −8.74° N, longitude = −121.14° E). b – d , No frost in an early-morning observation ( b ) and no frost in afternoon observations ( c , d ) during late southern spring in MY 36. The spectral profile along the black line in a is shown in e and reveals a marked increase in reflectance up to 20% in the BLU filter when frost is present. Errors are from the uncertainty in the absolute calibration of the instrument and are about ~3% (ref. 43 ). The illumination direction is indicated by the arrows in the bottom right corner of each image. North is up in all panels. The CaSSIS image IDs are shown in order ( a – d ): MY35_008465_192_0_NPB, MY36_020297_350_3_NPB, MY36_020366_190_1_NPB and MY36_020478_190_3_NPB. Credit: a , ESA/TGO/CaSSIS under a Creative Commons license CC-BY-SA 3.0 IGO .

CaSSIS observations of Olympus and Arsia Montes indicate diurnal and possibly seasonal trends in frost deposition (Fig. 3 ). The four detections in Olympus Mons (Fig. 3a,b ) are clustered around the early-morning hours ( lst   =  ~7:00–7:30) and northern spring equinox (Ls = ~320–40°). Similarly, the four detections in Arsia Mons (Fig. 3c–d ) fall within a slightly wider time range ( lst  = ~ 7:00–8:30) but around the southern winter solstice (Ls = ~45–145°). The early-morning non-detections in Arsia Mons fall within the southern summer period, which suggests seasonality (Extended Data Fig. 6b ), but the lack of early-morning observations in the northern summer precludes us from making the same conclusion for the detections in Olympus Mons (Extended Data Fig. 6a ). We removed observations at extremely high solar incidence angles (>85°) because of low image signal-to-noise ratio (SNR), and therefore there is an observational bias towards lst s at about 6:00 ( Methods ). Collectively, CaSSIS observations suggest that the frost cycle over Martian volcanoes is ephemeral and exhibits variability on multiple timescales. It appears to be influenced by diurnal patterns, probably reflecting daily temperature fluctuations. In addition, there is a probable control by the Martian seasons, indicating a longer-term variation in the frost cycle. On the basis of the CaSSIS observations, while there are indications of diurnal and seasonal influences on frost deposition on Martian volcanoes, these observations alone cannot definitively determine the composition of the frost. Therefore, we use simulations of surface temperatures as a proxy for frost composition.

a – d , Rose diagrams showing the seasonal ( a , c ) and diurnal ( b , d ) frost detections by CaSSIS over Olympus Mons ( a , b ) and Arsia Mons ( c , d ). The width of each bin reflects the number of CaSSIS observations. Frost is detected around northern spring equinox (Ls = ~0°) on Olympus Mons and around southern winter solstice (Ls = ~90°) on Arsia Mons. Frost is detected only in the early-morning hours (~7:00–8:00  lst ). The negative detections in the early morning bins correspond to observations that were acquired in warmer seasons.

Surface temperatures indicate water frost

At the time of CaSSIS frost detections in Olympus Mons (Fig. 1 ) and Arsia Mons (Fig. 2 ), the surface temperatures calculated by the general circulation model (GCM 46 ) via the Mars Weather Research and Forecasting (WRF 47 ) model are inconsistent with CO 2 frost. The stability of CO 2 frost at higher altitudes necessitates exceptionally low temperatures, specifically below 140 K, to maintain its solid state 30 . The predicted surface temperatures (at ~150 km model resolution) are ~150 K and 185 K at ~7:00  lst in Olympus Mons and at ~8:00  lst in Arsia Mons, respectively (Fig. 4 ). In addition, advanced high-resolution mesoscale modelling, with a model resolution of 5.47 km, reveals a substantial temperature difference between the surface temperature and the local CO 2 frost point at the locations of CaSSIS observations, with a difference of approximately 10 K at Olympus Mons (Fig. 5d ) and over 55 K at Arsia Mons (Extended Data Fig. 7d ). In fact, the surface temperatures predicted at each CaSSIS frost location (Table 1 ) consistently exceed the CO 2 frost point, corresponding to the mean surface temperature ~162 K (excluding C3 and C6). The stratification of water vapour in Mars’s atmosphere, especially near the surface, is not well understood 48 , making the determination of the H 2 O frost point challenging due to its considerable variability; however, it is generally accepted that this point occurs at around 180 K (ref. 14 ). Since the predicted surface temperatures at the time of CaSSIS, HRSC and NOMAD observations are too warm, this suggests that CO 2 frost is unlikely, hence providing support for the presence of water frost. At these seasons (Ls = 346.7° for Olympus Mons and Ls = 93.8° for Arsia Mons), CO 2 frost was also not observed by the Thermal Emission Imaging System 29 or by the Emirates Mars InfraRed Spectrometer 32 . Interestingly, the GCM also predicts that some CO 2 frost may be present at Ls = ~0–150° and at around sunrise (5:00–6:00  lst ) in Arsia Mons (Fig. 4b ). This result is consistent with previous studies indicating CO 2 frost formation from minutes to tens of minutes after sunrise in the equatorial regions 29 , 30 , 31 . However, such potential CO 2 frost deposits would sublime very quickly and would be difficult to detect by cameras and spectrometers due to low SNR 34 . In addition, we investigated the possible role of CO 2 frost in regolith gardening and slope streak formation on Mars 30 , 34 , 49 . We found no slope streaks on the calderas of the largest Tharsis volcanoes or any obvious differences in talus boulder shapes and sizes ( Methods and Extended Data Fig. 8 ). These results suggest that the diurnal CO 2 or H 2 O frost cycle plays a minor (if any) role in landscape evolution at these sites.

a , b , Annual surface temperatures at four different local mean solar times (LMST). c , d , Diurnal surface temperatures at Olympus Mons (Ls = 350°) ( c ) and Arsia Mons (Ls = 90°) ( d ) as predicted by the GCM. In c , d , blue and red horizontal dashed lines depict CO 2 30 and H 2 O frost point 14 , respectively. On both volcano calderas at the time of CaSSIS image acquisition, CO 2 frost point is not reached. This indicates favourable conditions for H 2 O ice. The simulations were conducted at geographical coordinates 18.75° N, −133.75° E for Olympus Mons and −8.75° N, −121.25 °E for Arsia Mons.

a – d , Utilizing MarsWRF high-resolution mesoscale modelling (at the time of CaSSIS observation Fig. 1d ), this figure presents the influence of Olympus Mons’s topography on its local climate, as shown by elevation gradients ( a ), surface atmospheric pressure ( b ), near-surface horizontal wind patterns ( c ) and the deviation in temperature between the Martian surface and the local CO 2 frost point ( d ). The topography of the Olympus Mons caldera is demonstrated to cause noticeable variations in local pressure, wind velocities and temperature gradients. The black outline across all panels highlights the boundary of the Olympus Mons caldera, while the black dashed rectangle marks the area observed by CaSSIS, as referenced in Fig. 1d . The CO 2 frost point in the area of CaSSIS observation is exceeded by about 10 K. By contrast, the CO 2 frost point in Arsia Mons is exceeded by around 60 K (Extended Data Fig. 7d ).

Microclimate and water ice amount

Our high-resolution mesoscale simulations reveal the distinct microclimatic conditions induced by the topography of the Tharsis volcanoes, as shown in Fig. 5 and Extended Data Fig. 7 . Specifically, within the calderas of Olympus Mons and Arsia Mons, we observe a substantial reduction in surface atmospheric pressure and near-surface horizontal wind speeds compared with the surrounding areas. For example, within the caldera of Olympus Mons (Fig. 5b ), the atmospheric pressure is estimated at only 110 Pa, compared with 160 Pa at the mountain’s base. Similarly, in the area of Arsia Mons (Extended Data Fig. 7b ), the pressure is about 100 Pa, notably lower than the over 200 Pa found in the adjacent plains. Moreover, the near-surface horizontal wind speeds within Olympus Mons (Fig. 5c ) are estimated at less than 10 m s –1 , in stark contrast to the approximately 30 m s –1 observed along the volcano’s flanks. In the case of Arsia Mons (Extended Data Fig. 7c ), the wind speeds are below 5 m s –1 within the caldera, compared with roughly 20 m s –1 on the flanks, highlighting the profound impact of volcanic topography on localized weather patterns.

Furthermore, our GCM simulations suggest that the thickness of water frost deposits is on the order of 1 µm ( Methods ). However, this estimate carries considerable uncertainty due to the unknown quantities of water-vapour-column abundances. To refine this estimate, we reference radiative transfer calculations 50 , 51 , which suggest a minimum thickness of 100 µm, while laboratory experiments 52 imply a thickness of about 10 µm ( Methods ). By adopting the median thickness of 10 µm for the water frost, and considering that the frost deposits are confined to the calderas of Olympus, Arsia, Ascraeus Montes and Ceraunius Tholus, we estimate that there is a transfer of approximately 1.5 × 10 8  kg of water ice between the surface and the atmosphere ( Methods ).

Possible sources of water vapour

The seasonal trends as shown by the set ( n  = 13) of CaSSIS observations suggests an atmospheric phenomenon driven by water transport due to large-scale seasonal changes, such as sublimation of the seasonal ice cap in the opposite hemisphere and transportation of humid air into the volcano calderas by upslope winds. Seasonal processes have been observed at a wide range of Martian latitudes 53 and may also apply to the Tharsis region. For example, the activity of the Aphelion Cloud Belt peaks at Ls ∼ 40°–140° (ref. 54 ), and in general little cloud activity is observed at Ls ~245°–320° 10 . Similarly, afternoon orographic clouds have been detected by Mars Reconnaissance Orbiter’s Mars Color Imager 55 over the Tharsis volcanoes 10 . The seasonal observation of water-vapour enrichment over Tharsis 17 shows increased abundances around northern spring equinox (Ls 0°), consistent with the CaSSIS detections of frost close to this season in Olympus Mons. Therefore, we hypothesize that this water-vapour enrichment 17 may be the source of the frost deposits detected in our study. The transport of water vapour from high latitudes to the Tharsis highlands could be facilitated by large-scale atmospheric eddies 56 . This process could be further augmented by strong upslope winds, driven by a combination of thermal effects and mountain gravity waves 57 , facilitating the movement of moisture over the volcano calderas. The local topography-induced circulation 57 and microclimatic conditions within the caldera (shown in Fig. 5 and Extended Data Fig. 7 ) may create favourable conditions for water frost condensation during the cold Martian nights. Within these calderas, ~150,000 tons of water ice is exchanged daily between the regolith and the atmosphere during the cold Martian seasons. Although this amount is relatively a small fraction of the seasonal inventory of water vapour in the Martian atmosphere (~10 12  kg) (ref. 14 ), it is important in the context of localized Martian environmental processes. Understanding these micro-environments is crucial for a comprehensive understanding of Mars’s hydrological cycle.

It is conceivable that dormant volcanoes can emit CO 2 , water vapour and minor amounts of SO 2 (ref. 58 ) via diffuse outgassing from the regolith 59 , 60 . If the observed water frost deposits are of volcanic origin, their distribution may constrain models for present-day outgassing from the interior. However, on Mars, SO 2 has not been detected 61 and no thermal hotspots have been found 62 . A volcanic source for the condensate cannot completely be ruled out, but further tests for trace species (CO 2 , H 2 S and SO 2 ) would be useful to explore the likelihood of this potential mechanism. Consequently, we conclude here that the newly detected frosts on Tharsis volcano calderas are probably of atmospheric origin.

CaSSIS frost observations

We surveyed ~4,200 CaSSIS images (acquired up to 2022 February 05) with illumination geometries of 50–90° incidence within dusty, low thermal inertia (<100 TIU) regions (60° N—30° S). Only images that include the latest CaSSIS radiometric and absolute calibration were used in this study 43 , 63 , 64 .

The images used in this study consisted of early (6:00–9:00  lst ) and late (15:00–18:00  lst ) times. Analysis and comparison in these two local time regimes may help the distinction between early-morning and late-afternoon phenomena. During the survey, it was noticed that most CaSSIS images acquired at extremely high solar incidence angles of 85–90° contain colour and calibration artefacts due to the decrease in SNR and/or an increase in aerosol contribution from the atmosphere 63 . Consequently, the images with colour artefacts were labelled as ambiguous and were not used for further analysis.

Frost detections relied on the use of CaSSIS NPB (near infrared (NIR) = 940, panchromatic (PAN) = 670, blue (BLU) = 497 nm) and synthetic RGB (red–green–blue; PAN and BLU only) products. These filter configurations allow a convenient separation between frosty and frost-free terrains. In CaSSIS colour products, frosty areas appear bluish, and/or whitish, and sometimes are bright only in the BLU filter (relative to frost-free areas; also see Supplementary Figs. 9 and 10 ). In support, we observe bluish frost deposits in HRSC colour images shown in Fig. 1b and Extended Data Fig. 1 (composites of blue (440 nm), green (530 nm) and red (750 nm) channels).

As shown by previous studies 21 , 65 deposits are usually correlated with topography (prefer poleward-sloping terrains). Therefore, if both conditions were met (colour and topographic correlation), it was considered a strong indication of surface frost. As a final procedure, each of these candidate detections was then analysed using a spectral profile tool in the Environment for Visualizing Images software. This procedure extracts the pixel irradiance over flux ( I/F ) values between two manually selected points crossing the potentially frosted region in each filter. The profiles were then normalized by a mean I/F of a nearby frost-free, relatively flat region of interest (ROI), a well-established method to cancel out some of the atmospheric and topographic effects 49 , 66 , 67 , 68 , 69 , 70 . If the frost deposits were brighter in the BLU filter than the surrounding frost-free terrains by at least 3% (within CaSSIS absolute uncertainty 43 ), then such images were flagged as potential frost detections. This survey yielded many frosty sites (not shown here) at latitudes ~40° N and ~30° S. However, because these latitude bands are dominated by known seasonal frost deposits 21 , 23 , 65 and we do not have a robust method to distinguish between seasonal and diurnal frost, we further narrowed our filtering criteria. The final frost detections analysed here were restricted to equatorial ~20° N to ~10° S latitudes (outside of the seasonal mid-latitude regions). In this work, only equatorial sites that included visible evidence of frost are considered.

The spectral profile shown in Fig. 2e was computed by dividing each pixel along the profile by an average pixel value extracted from an ROI in Extended Data Fig. 5d . The ROI (>100 pixels in size) was selected on a frost-free and relatively flat terrain as suggested by the low slope values in the CaSSIS digital elevation model of this site. CaSSIS digital elevation models were produced by a pipeline developed at the Astronomical Observatory of Padova, National Institute for Astrophysics 71 , 72 .

NOMAD-LNO spectral processing

The NOMAD instrument is a suite of three high-resolution spectrometers also on board TGO, offering nadir infrared observations through its LNO channel 37 , 73 . This channel covers the 2.2–3.8 µm spectral range where several spectral features of ice are distributed over different wavelengths. Nevertheless, the NOMAD-LNO spectrometer has the particularity of not observing the entire spectral range at once. The data are acquired through small spectral windows, representing specific diffraction orders of the diffraction grating. Each LNO observation can select a maximum number of 6 diffraction orders every 15 seconds to ensure the best possible SNR 74 , 75 , 76 . The LNO footprint (instantaneous field of view) is 17.5 km × 0.5 km (ref. 75 ), which provides enough spatial scale to resolve the caldera of Olympus Mons. In this work, we use spectrally and radiometrically calibrated LNO data converted into a reflectance factor. The 2.7 µm ice band is the strongest in the LNO spectral range, resulting from both CO 2 and H 2 O ice absorption. Although the use of this band is not suitable for quantifying the amount of ice (easily saturated), it is effective for detecting homogeneous deposits (both CO 2 and H 2 O ice), as demonstrated with the ice index value 77 . This spectral parameter uses two diffraction orders. It is based on the combination of high reflectivity at continuum wavelengths with a more pronounced absorption in the 2.7 μm band. Initially defined as the spectral ratio between the reflectance factors of order 190 (continuum part, 2.32–2.34 µm) and 169 (short wavelengths shoulder of the 2.7 µm band, 2.61–2.63 µm) (ref. 77 ), we adjust the ice index by considering the available orders of the joint CaSSIS–NOMAD observations, that is, orders 190 and 168 (2.64–2.65 µm).

In nadir mode, the variability in the reflectance factors is caused mainly by the surface albedo variations resulting from the different absorption of the Martian surface mineralogy 78 , 79 , 80 . To remove spatial albedo variations over the explored Martian surface, we normalize the LNO reflectance factors to the Martian albedo. The adjusted ice index (II) can thus be defined as:

where R i is the LNO reflectance factor value averaged around the central wavelength i of the LNO spectrum, fitted by a third-degree polynomial to mitigate the spectral oscillations resulting from the instrumental characteristics of the LNO channel, which become significant on the edges of each order (Supplementary Figs. 1 and 2 ). OMEGA i is the OMEGA albedo map 80 based on reflectance spectra in the near infrared as NOMAD-LNO R i . Two OMEGA albedo maps are used in this work: one defined at 2.32 µm for order 190 and the other defined at 2.62 µm for order 168. Studies have shown that this spectral parameter identifies spatially extensive and abundant ice deposits when the index values are three sigma higher than their average value over ice-free mid-latitude terrain 77 , 81 .

Mars GCM modelling

We perform the Martian GCM simulation for the entire MY 36 using the MarsWRF model, which is the Mars adaptation of the general-purpose planetary atmosphere model, planetWRF 47 . Here the GCM set-up is based on a previous study 46 examining the Martian planetary boundary and dust–turbulence interaction over a decade, from MY 24 to MY 34, which hosted three global dust storms. The reference model set-up 46 was validated against NASA’s Mars Climate Sounder (MCS) observations on board the Mars Reconnaissance Orbiter, radio occultation observations from ESA’s Mars Express orbiter, as well as the in situ observations from NASA’s Mars Science Laboratory Curiosity rover. This model set-up consists of a semi-interactive two-moment dust transport model 46 within the MarsWRF framework, in a way that the dust is lifted, mixed by model winds and sedimented, as guided by observed maps of column-integrated dust optical thickness 82 , 83 . Via this method, model processes govern the vertical dust distribution and related dust radiative heating, yet the horizontal dust distribution is guided to match the orbiter observations. In this model, the horizontal dust distribution is constrained to follow observations. In this model, the two-stream correlated k -distribution scheme is used for the short-wave and long-wave radiative transfer 84 . We use a Mars-specific boundary-layer turbulence parameterization scheme, which allows us to obtain the surface–atmosphere exchange coefficients 85 Surface properties of the MarsWRF model, such as the topography, albedo, emissivity and thermal inertia, are acquired from the datasets of the Mars Orbiter Laser Altimeter 2 and Thermal Emission Spectrometer (TES 78 ) observations, where the details are presented in another study 47 . Here we increased the horizontal model grid spacing of the GCM from 5° × 5° to 2.5° × 2.5° (ref. 46 ), enabling better spatial coverage to provide more realistic boundary and initial conditions to our mesoscale simulations. We used 52 vertical sigma layers extending up to the model top of 100 km. The predicted surface temperatures are shown in Table 1.

Our modelling methodology is based on a previous study by MarsWRF 85 , 86 . Mesoscale simulations for Fig. 5 and Extended Data Fig. 7 were forced with initial and boundary conditions acquired by GCM simulations corresponding to the same seasonal conditions of CaSSIS observations shown in Figs. 1 and 2 . The plots we present in terms of winds, pressure and temperature correspond to the local hours of observations. We nested three mesoscale domains in our GCM domain (see Supplementary Fig. 12 for details). Mesoscale domains use prescribed boundary conditions, derived either from GCM predictions (as in the case of d2) or from another mesoscale domain (d3 and d4). The GCM grid has a horizontal resolution of approximately 150 km. We progressively increased the horizontal resolution with a factor of three for our nested mesoscale domains. Our innermost domain, d4, has a horizontal resolution of 5.47 km. To assess the accuracy of our mesoscale predictions, we compared MarsWRF surface temperature predictions with the surface temperature observations by MCS and TES available for Olympus Mons and Arsia Mons regions at around 3:00  lst (Supplementary Fig. 13 ). We considered a sufficient Ls range of MCS and TES observations (Ls 310–360 for Olympus Mons and Ls 75–100 for Arsia Mons) to provide a sufficient set of observations to acquire a temperature map to be compared with MarsWRF simulations. These observations range from 1:00  lst to 4:00  lst , and MarsWRF estimations at the corresponding local times are compared for validation. The modelled surface temperatures for Olympus Mons caldera are within 10 K of the observations and within a few degrees Kelvin for Arsia Mons. It is important to note that these predictions carry uncertainties, particularly in regions with complex topography such as the Tharsis volcanoes.

Surface frost thickness and mass estimations

The MarsWRF GCM incorporates the phase transition and transport mechanisms of water vapour and ice, facilitating a parameterization of the Martian hydrological cycle that aligns with the methodologies outlined by previous studies 87 . This parameterization enables the model to approximate the surface frost layer thickness to about 1 μm at the locations in our study. However, it is important to acknowledge the inherent uncertainties associated with such estimations, particularly due to the limitations of physical parameterizations within Martian atmospheric models. These uncertainties are most pronounced in the prediction of atmospheric variables in regions lacking empirical observational data, such as the deposition rates of atmospheric volatiles.

In a recent experimental investigation, one study 52 systematically evaluated the interaction between water frost deposition and the optical properties of a Martian soil simulant, specifically Mars Global Simulant (MGS-1 88 ). The experimental design involved the controlled deposition of water frost on the surface of the simulant, followed by precise measurements of both the spectral reflectance and the thickness of the frost layer. The findings indicate that a frost layer thickness ranging from approximately 10 to 20 μm is required to significantly attenuate the characteristic red slope of the spectral reflectance, aligning with the observed morning frost brightening in the blue wavelengths by approximately 10–20% as detected by the CaSSIS instrument. Furthermore, the study demonstrates that a relatively thin frost layer of about 100 μm is sufficient to flatten the visible spectrum, effectively neutralizing the spectral features.

Radiative transfer models 50 , 51 can provide an additional constraint on the frost thickness estimation via the minimum optical depth ( τ ) necessary for frost visibility at CaSSIS visible and LNO near-infrared wavelengths. For example, with a τ of 10 –2 , we anticipate a minimal impact on albedo, less than 0.1 at CaSSIS visible wavelengths and negligible at LNO near-infrared wavelengths, given the single-scattering co-albedo is around 10 −6 for visible light and less than 10 −1 at 2.6 μm. However, LNO observations indicate a discernible albedo reduction at near-infrared wavelengths, suggesting a higher optical depth than 10 −2 . This implies that the frost’s grain radius and/or thickness must exceed 5 μm and 1 μm, respectively. If the grain radius is about 1 μm, then the frost layer’s thickness could be significantly greater, approximately 100 μm.

To conduct a preliminary quantification of the frost mass, we assumed a uniform frost layer thickness across all identified frost-covered regions, as observed by CaSSIS. The geographical extent of the frost coverage was approximated to the combined surface areas of the calderas of Martian volcanoes such as Arsia Mons, Olympus Mons, Ascraeus Mons and Ceraunius Tholus. By integrating the uniform frost thickness with the delineated area and adopting the density value for pure ice, we derived an initial estimate of the total frost mass. This approach provides a rudimentary yet insightful approximation of the frost mass, acknowledging the broad-scale estimative nature of this calculation.

Boulder size measurements

To investigate a potential effect of the diurnal frost cycle on the overall geomorphology and landscape evolution, we studied the shape of mass-wasted boulders across six sites of interest. Here we compare the sizes of boulders on volcanoes with frost as determined by CaSSIS (two sites in Olympus Mons and one in Arsia Mons) and on volcanoes where frost has not been detected (Tharsis Mons, Jovis Tholus and Ulysses Tholus). Because frost accumulates preferentially on poleward-facing slopes on Mars 29 , here we focused only on north-facing and south-facing slopes. This might reveal whether there are considerable differences in boulder sizes due to frost weathering 89 .

We used eight map-projected High Resolution Imaging Science Experiment (HiRISE) 90 images in Geographic Information System (QGIS) to determine the three principal dimensions of each identified boulder. The first dimension is defined as the longest distance between two points on the boulder as visible from orbit. Similarly, the second dimension is defined as the diameter of the boulder orthogonal to the first dimension. Last, the third dimension is defined as the height of the boulder as estimated using shadow length and solar incidence angle. In total, we identified and measured 63 boulders across the six sites. All derived measurements were plotted on ternary diagrams 91 using the Tri-Plot software 92 . These diagrams relate the three principal dimensions of each boulder, visualizing its overall shape as well as similarities and differences within and across the studied sites.

Data availability

CaSSIS data can be found on the University of Bern repository ( https://observations.cassis.unibe.ch/ ) and the ESA’s Planetary Science Archive ( https://archives.esac.esa.int/psa ). NOMAD-LNO observations are also found on the ESA’s Planetary Science Archive.

Code availability

The PlanetWRF model for Martian GCM and mesoscale simulations is accessible by request at https://planetwrf.com/ .

Carr, M. H. Tectonism and volcanism of the Tharsis region of Mars. J. Geophys. Res. 79 , 3943–3949 (1974).

Article   Google Scholar  

Smith, D. E. et al. Mars Orbiter Laser Altimeter: experiment summary after the first year of global mapping of Mars. J. Geophys. Res. Planets 106 , 23689–23722 (2001).

Plescia, J. B. Morphometric properties of Martian volcanoes. J. Geophys. Res. Planets 109 , E03003 (2004).

Neukum, G. et al. Recent and episodic volcanic and glacial activity on Mars revealed by the High Resolution Stereo Camera. Nature 432 , 971–979 (2004).

Article   CAS   Google Scholar  

Giardini, D. et al. The seismicity of Mars. Nat. Geosci. 13 , 205–212 (2020).

Stähler, S. C. et al. Tectonics of Cerberus Fossae unveiled by marsquakes. Nat. Astron. 6 , 1376–1386 (2022).

Broquet, A. & Andrews-Hanna, J. C. Geophysical evidence for an active mantle plume underneath Elysium Planitia on Mars. Nat. Astron. 7 , 160–169 (2023).

Google Scholar  

Curran, R. J., Conrath, B. J., Hanel, R. A., Kunde, V. G. & Pearl, J. C. Mars: Mariner 9 spectroscopic evidence for H 2 O ice clouds. Science 182 , 381–383 (1973).

Kahn, R. The spatial and seasonal distribution of Martian clouds and some meteorological implications. J. Geophys. Res. Space Phys. 89 , 6671–6688 (1984).

Benson, J. L., James, P. B., Cantor, B. A. & Remigio, R. Interannual variability of water ice clouds over major Martian volcanoes observed by MOC. Icarus 184 , 365–371 (2006).

Hernández-Bernal, J. et al. An extremely elongated cloud over Arsia Mons volcano on Mars: I. Life cycle. J. Geophys. Res. Planets 126 , e2020JE006517 (2021).

Fernando, A. M., Wolff, M. J. & Forget, F. Seasonal variations of orographic clouds on Mars with MRO/MARCI observations and the Mars Planetary Climate Model. Icarus 400 , 115559 (2023).

Houben, H., Haberle, R. M., Young, R. E. & Zent, A. P. Modeling the Martian seasonal water cycle. J. Geophys. Res. Planets 102 , 9069–9083 (1997).

Montmessin, F., Smith, M. D., Langevin, Y., Mellon, M. T. & Fedorova, A. in The Atmosphere and Climate of Mars (eds Clancy, R. T. et al.) 338–373 (Cambridge Univ. Press, 2017); https://doi.org/10.1017/9781139060172.011

Montmessin, F., Forget, F., Rannou, P., Cabane, M. & Haberle, R. M. Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model. J. Geophys. Res. Planets 109 , E10004 (2004).

Titov, D. V. et al. Observations of water vapour anomaly above Tharsis volcanoes on Mars in the ISM (Phobos-2) experiment. Planet. Space Sci. 42 , 1001–1010 (1994).

Maltagliati, L. et al. Observations of atmospheric water vapor above the Tharsis volcanoes on Mars with the OMEGA/MEx imaging spectrometer. Icarus 194 , 53–64 (2008).

Jones, K. L. et al. One Mars year: Viking lander imaging observations. Science 204 , 799–806 (1979).

Hart, H. M. & Jakosky, B. M. Composition and stability of the condensate observed at the Viking lander 2 site on Mars. Icarus 66 , 134–142 (1986).

Svitek, T. & Murray, B. Winter frost at Viking lander 2 site. J. Geophys. Res. Solid Earth 95 , 1495–1510 (1990).

Carrozzo, F. G., Bellucci, G., Altieri, F., D’Aversa, E. & Bibring, J.-P. Mapping of water frost and ice at low latitudes on Mars. Icarus 203 , 406–420 (2009).

Schorghofer, N. & Edgett, K. S. Seasonal surface frost at low latitudes on Mars. Icarus 180 , 321–334 (2006).

Vincendon, M. et al. Near-tropical subsurface ice on Mars. Geophys. Res. Lett . 37 , L01202 (2010).

Piqueux, S. et al. Mars thermal inertia and surface temperatures by the Mars Climate Sounder. Icarus https://doi.org/10.1016/j.icarus.2023.115851 (2023).

Fedorova, A. et al. Mars water vapor abundance from SPICAM IR spectrometer: seasonal and geographic distributions. J. Geophys. Res. Planets 111 , E09S08 (2006).

Davies, D. W. The relative humidity of Mars’ atmosphere. J. Geophys. Res. Solid Earth 84 , 8335–8340 (1979).

Jakosky, B. M. The seasonal cycle of water on Mars. Space Sci. Rev. 41 , 131–200 (1985).

Landis, G. A. Observation of frost at the equator of Mars by the Opportunity rover. In Proc. 38th Annu. Lunar Planet. Sci. Conf . abstr. 2433 (2007).

Khuller, A. R., Christensen, P. R., Harrison, T. N. & Diniega, S. The distribution of frosts on Mars: links to present-day gully activity. J. Geophys. Res. Planets 126 , e2020JE006577 (2021).

Piqueux, S. et al. Discovery of a widespread low-latitude diurnal CO 2 frost cycle on Mars. J. Geophys. Res. Planets 121 , 1174–1189 (2016).

Cushing, G. E. & Titus, T. N. MGS-TES thermal inertia study of the Arsia Mons caldera. J. Geophys. Res. Planets 113 , E06006 (2008).

Stcherbinine, A. et al. Diurnal and seasonal mapping of Martian ices with EMIRS. Geophys. Res. Lett. 50 , e2023GL103629 (2023).

Christensen, P. R. et al. in 2001 Mars Odyssey (ed. Russell, C. T.) 85–130 (Springer, 2004); https://doi.org/10.1007/978-0-306-48600-5_3

Lange, L., Piqueux, S. & Edwards, C. S. Gardening of the Martian regolith by diurnal CO 2 frost and the formation of slope streaks. J. Geophys. Res. Planets 127 , e2021JE006988 (2022).

Thomas, N. et al. The Colour and Stereo Surface Imaging System (CaSSIS) for the ExoMars Trace Gas Orbiter. Space Sci. Rev. 212 , 1897–1944 (2017).

Neukum, G., Jaumann, R. & the HRSC Co-Investigator and Experiment Team. HRSC: the high resolution stereo camera of Mars Express. ESA 1240 , 17–35 (2024).

Vandaele, A. C. et al. NOMAD, an integrated suite of three spectrometers for the ExoMars Trace Gas Mission: technical description, science objectives and expected performance. Space Sci. Rev. 214 , 80 (2018).

Hapke, B. Theory of Reflectance and Emittance Spectroscopy (Cambridge Univ. Press, 2012); https://doi.org/10.1017/CBO9781139025683

Malin, M. C. et al. Context Camera Investigation on board the Mars Reconnaissance Orbiter. J. Geophys. Res. Planets 112 , E05S04 (2007).

Presley, M. & Christensen, P. Thermal conductivity measurements of particulate materials: 4. Effect of bulk density for granular particles. J. Geophys. Res . 115 , E07003 (2010).

Christensen, P. R. Martian dust mantling and surface composition: interpretation of thermophysical properties. J. Geophys. Res. Solid Earth 87 , 9985–9998 (1982).

Presley, M. A. & Christensen, P. R. Thermal conductivity measurements of particulate materials 2. Results. J. Geophys. Res. Planets 102 , 6551–6566 (1997).

Thomas, N. et al. Absolute calibration of the Colour and Stereo Surface Imaging System (CaSSIS). Planet. Space Sci. 211 , 105394 (2022).

Marzo, G. A., Roush, T. L., Blanco, A., Fonti, S. & Orofino, V. Cluster analysis of planetary remote sensing spectral data. J. Geophys. Res. Planets 111 , E03002 (2006).

Pajola, M. et al. Lermontov crater on Mercury: geology, morphology and spectral properties of the coexisting hollows and pyroclastic deposits. Planet. Space Sci. 195 , 105136 (2021).

Senel, C. B. et al. Interannual, seasonal and regional variations in the Martian convective boundary layer derived from GCM simulations with a semi-interactive dust transport model. J. Geophys. Res. Planets 126 , e2021JE006965 (2021).

Richardson, M. I., Toigo, A. D. & Newman, C. E. PlanetWRF: a general purpose, local to global numerical model for planetary atmospheric and climate dynamics. J. Geophys. Res. Planets 112 , E09001 (2007).

Tamppari, L. K. & Lemmon, M. T. Near-surface atmospheric water vapor enhancement at the Mars Phoenix lander site. Icarus 343 , 113624 (2020).

Valantinas, A. et al. CaSSIS color and multi-angular observations of Martian slope streaks. Planet. Space Sci. 209 , 105373 (2021).

Wiscombe, W. J. & Warren, S. G. A model for the spectral albedo of snow. I: pure snow. J. Atmos. Sci. 37 , 2712–2733 (1980).

Khuller, A. R., Christensen, P. R. & Warren, S. G. Spectral albedo of dusty Martian H 2 O snow and ice. J. Geophys. Res. Planets 126 , e2021JE006910 (2021).

Spadaccia, S., Patty, C. H. L., Thomas, N. & Pommerol, A. Experimental study of frost detectability on planetary surfaces using multicolor photometry and polarimetry. Icarus 396 , 115503 (2023).

Dundas, C. M. et al. Active Mars: a dynamic world. J. Geophys. Res. Planets 126 , e2021JE006876 (2021).

Clancy, R. T. et al. in The Atmosphere and Climate of Mars (eds. Clancy, R. T. et al.) 76–105 (Cambridge Univ. Press, 2017); https://doi.org/10.1017/9781139060172.005

Bell, J. F. III et al. Mars Reconnaissance Orbiter Mars Color Imager (MARCI): instrument description, calibration, and performance. J. Geophys. Res. Planets 114 , E08S92 (2009).

Greybush, S. J., Gillespie, H. E. & Wilson, R. J. Transient eddies in the TES/MCS Ensemble Mars Atmosphere Reanalysis System (EMARS). Icarus 317 , 158–181 (2019).

Rafkin, S. C. R., Sta. Maria, M. R. V. & Michaels, T. I. Simulation of the atmospheric thermal circulation of a Martian volcano using a mesoscale numerical model. Nature 419 , 697–699 (2002).

Symonds, R. B., Rose, W. I., Bluth, G. J. S. & Gerlach, T. M. in Volatiles in Magmas (eds. Carroll, M. R. & Holloway, J. R.) 1–66 (De Gruyter, 1994); https://doi.org/10.1515/9781501509674-007

Hernández, P. et al. Soil gas CO 2 , CH 4 , and H 2 distribution in and around Las Cañadas caldera, Tenerife, Canary Islands, Spain. J. Volcanol. Geotherm. Res. 103 , 425–438 (2000).

Chiodini, G. et al. Fumarolic and diffuse soil degassing west of Mount Epomeo, Ischia, Italy. J. Volcanol. Geotherm. Res. 133 , 291–309 (2004).

Braude, A. S. et al. No detection of SO 2 , H 2 S, or OCS in the atmosphere of Mars from the first two Martian years of observations from TGO/ACS. Astron. Astrophys. 658 , A86 (2022).

Christensen, P. R. et al. Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results. Science 300 , 2056–2061 (2003).

Pommerol, A. et al. In-flight radiometric calibration of the ExoMars TGO Colour and Stereo Surface Imaging System. Planet. Space Sci. 223 , 105580 (2022).

Almeida, M. et al. Targeting and image acquisition of Martian surface features with TGO/CaSSIS. Planet. Space Sci. 231 , 105697 (2023).

Vincendon, M., Forget, F. & Mustard, J. Water ice at low to midlatitudes on Mars. J. Geophys. Res. Planets 115 , E10001 (2010).

Daubar, I. J. et al. Changes in blast zone albedo patterns around new Martian impact craters. Icarus 267 , 86–105 (2016).

Schaefer, E. I., McEwen, A. S. & Sutton, S. S. A case study of recurring slope lineae (RSL) at Tivat crater: implications for RSL origins. Icarus 317 , 621–648 (2019).

Munaretto, G. et al. Implications for the origin and evolution of Martian recurring slope lineae at Hale crater from CaSSIS observations. Planet. Space Sci. 187 , 104947 (2020).

Munaretto, G. et al. Topographic correction of HiRISE and CaSSIS images: validation and application to color observations of Martian albedo features. Planet. Space Sci. 200 , 105198 (2021).

Munaretto, G. et al. Multiband photometry of Martian recurring slope lineae (RSL) and dust-removed features at Horowitz crater, Mars from TGO/CaSSIS color observations. Planet. Space Sci. 214 , 105443 (2022).

Simioni, E. et al. 3DPD: a photogrammetric pipeline for a PUSH frame stereo cameras. Planet. Space Sci. 198 , 105165 (2021).

Re, C. et al. CaSSIS-based stereo products for Mars after three years in orbit. Planet. Space Sci. 219 , 105515 (2022).

Neefs, E. et al. NOMAD spectrometer on the ExoMars Trace Gas Orbiter mission: part 1—design, manufacturing and testing of the infrared channels. Appl. Opt. 54 , 8494–8520 (2015).

Thomas, I. R. et al. Optical and radiometric models of the NOMAD instrument part II: the infrared channels—SO and LNO. Opt. Express 24 , 3790–3805 (2016).

Thomas, I. R. et al. Calibration of NOMAD on ESA’s ExoMars Trace Gas Orbiter: part 2—the limb, nadir and occultation (LNO) channel. Planet. Space Sci. 218 , 105410 (2022).

Liuzzi, G. et al. Methane on Mars: new insights into the sensitivity of CH 4 with the NOMAD/ExoMars spectrometer through its first in-flight calibration. Icarus 321 , 671–690 (2019).

Oliva, F. et al. Martian CO 2 ice observation at high spectral resolution with ExoMars/TGO NOMAD. J. Geophys. Res. Planets 127 , e2021JE007083 (2022).

Christensen, P. R. et al. Mars Global Surveyor Thermal Emission Spectrometer experiment: investigation description and surface science results. J. Geophys. Res. Planets 106 , 23823–23871 (2001).

Viviano-Beck, C. E. et al. Revised CRISM spectral parameters and summary products based on the currently detected mineral diversity on Mars. J. Geophys. Res. Planets 119 , 1403–1431 (2014).

Riu, L. et al. The M3 project: 1—a global hyperspectral image-cube of the Martian surface. Icarus 319 , 281–292 (2019).

Ruiz Lozano, L. et al. Evaluation of the capability of ExoMars-TGO NOMAD infrared nadir channel for water ice clouds detection on Mars. Remote Sens. https://doi.org/10.3390/rs14174143 (2022).

Montabone, L. et al. Eight-year climatology of dust optical depth on Mars. Icarus 251 , 65–95 (2015).

Montabone, L. et al. Martian year 34 column dust climatology from Mars climate sounder observations: reconstructed maps and model simulations. J. Geophys. Res. Planets 125 , e2019JE006111 (2020).

Mischna, M. A., Lee, C. & Richardson, M. Development of a fast, accurate radiative transfer model for the Martian atmosphere, past and present. J. Geophys. Res. Planets 117 , E10009 (2012).

Temel, O. et al. Large eddy simulations of the Martian convective boundary layer: towards developing a new planetary boundary layer scheme. Atmos. Res. 250 , 105381 (2021).

Temel, O. et al. Strong seasonal and regional variations in the evaporation rate of liquid water on Mars. J. Geophys. Res. Planets 126 , e2021JE006867 (2021).

Richardson, M. I. & Wilson, R. J. Investigation of the nature and stability of the Martian seasonal water cycle with a general circulation model. J. Geophys. Res. Planets 107 , 7–28 (2002).

Cannon, K. M., Britt, D. T., Smith, T. M., Fritsche, R. F. & Batcheldor, D. Mars global simulant MGS-1: a Rocknest-based open standard for basaltic Martian regolith simulants. Icarus 317 , 470–478 (2019).

Hales, T. C. & Roering, J. J. Climatic controls on frost cracking and implications for the evolution of bedrock landscapes. J. Geophys. Res. Earth Surf . 112 , F02033 (2007).

McEwen, A. S. et al. Mars Reconnaissance Orbiter’s High Resolution Imaging Science Experiment (HiRISE). J. Geophys. Res. 112 , E05S02 (2007).

Sneed, E. D. & Folk, R. L. Pebbles in the lower Colorado River, Texas: a study in particle morphogenesis. J. Geol. 66 , 114–150 (1958).

Graham, D. J. & Midgley, N. G. Graphical representation of particle shape using triangular diagrams: an Excel spreadsheet method. Earth Surf. Process. Landf. 25 , 1473–1477 (2000).

Download references

Acknowledgements

CaSSIS is a project of the University of Bern and funded through the Swiss Space Office via ESA’s PRODEX programme. The instrument hardware development was also supported by the Italian Space Agency (ASI) (ASI-INAF agreement no. 2020-17-HH.0), INAF/Astronomical Observatory of Padova and the Space Research Center (CBK) in Warsaw. Support from SGF (Budapest), the University of Arizona (Lunar and Planetary Lab.) and NASA is also gratefully acknowledged. Operations support from the UK Space Agency under grant ST/R003025/1 is also acknowledged. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS) and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493) and Italian Space Agency through grant 2018-2-HH.0. Operations and science support from the UK Space Agency under grants ST/X006549/1, ST/Y000234/1, ST/V005332/1 and ST/V002295/1 is also acknowledged. This research is financially supported by the Research Foundation-Flanders (FWO) with grant 12AM624N to C.B.S., and grant 12ZZL23N to O.T. J.J.L.-M. acknowledges financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033 and by Spanish MICIIN through Plan Nacional and European funds. F.S. acknowledges support from the Institut National des Sciences de l’Univers (INSU), the Centre National de la Recherche Scientifique (CNRS) and Centre National d’Etudes Spatiales (CNES) through the Programme National de Planétologie. MRELM acknowledges funding from the KU internal grant (8474000336-KU-SPSC).

Open access funding provided by University of Bern.

Author information

Authors and affiliations.

Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland

A. Valantinas, N. Thomas, A. Pommerol, M. Almeida & M. Read

Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI, USA

A. Valantinas

The Royal Observatory of Belgium (ROB-ORB), Brussels, Belgium

O. Karatekin, L. Ruiz Lozano, C. B. Senel & O. Temel

Archaeology, Environmental Changes & Geo-chemistry (AMGC) Research Unit, Vrije Universiteit Brussel, Brussels, Belgium

C. B. Senel

Institute of Astronomy, KU Leuven, Leuven, Belgium

Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany

E. Hauber & D. Tirsch

Center for Space and Habitability, University of Bern, Bern, Switzerland

V. T. Bickel

INAF-Osservatorio Astronomico di Padova, Padova, Italy

G. Munaretto, M. Pajola, C. Re & G. Cremonese

Istituto di Astrofisica e Planetologia Spaziali, IAPS-INAF, Rome, Italy

F. Oliva, F. G. Carrozzo, E. D’Aversa & G. Bellucci

GEOPS, Université Paris-Saclay, CNRS, Orsay, France

Institut Universitaire de France, Paris, France

Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium

I. Thomas, F. Daerden, B. Ristic & A. C. Vandaele

Lunar and Planetary Laboratory, University of Arizona, Tuscon, AZ, USA

A. S. McEwen

Institute for Earth and Space Exploration, Department of Earth Sciences, Western University, London, Ontario, Canada

V. G. Rangarajan

Space and Planetary Science Center and Department of Earth Sciences, Khalifa University, Abu Dhabi, United Arab Emirates

M. R. El-Maarry

School of Physical Sciences, The Open University, Milton Keynes, UK

M. R. Patel

Instituto de Astrofísica de Andalucia, Granada, Spain

J. J. Lopez-Moreno

You can also search for this author in PubMed   Google Scholar

Contributions

A.V. led conceptualization, CaSSIS data collection and analysis, and writing. N.T. and A.P. led conceptualization, design and production of the CaSSIS instrument and its operation. O.T., C.B.S. and O.K. performed mesoscale and global circulation model simulations with MarsWRF, did post-processing of the modelling results and compared model predictions with MCS and TES observations, which were analysed by O.T. and O.K. L.R.L. and F.O. performed NOMAD spectral analysis. G.M. and M.P. performed CaSSIS clustering analysis and photometry. V.T.B. processed HiRISE data, performed boulder size measurements and analyzed boulder shapes. L.R.L., V.T.B., G.M., M.P., F.S., A.P., A.S.M., M.R.E.-M., V.G.R., N.T. and I.T. contributed to writing. F.G.C., A.P., N.T., G.B. and E.D. contributed to discussions and assisted with data interpretation. C.R., G.B. and I.T. contributed to data processing. A.C.V., J.J.L.-M., F.D. and M.R.P. contributed to the design and production of the NOMAD instrument and its operation. D.T., E.H., M.R., M.A., I.T. and B.R. participated in instrument operations and planning of the observations. N.T. and G.C. acquired funds for the development of the CaSSIS instrument and the generation of DEMs. A.C.V. and F.D. acquired funds for the development of the NOMAD instrument.

Corresponding author

Correspondence to A. Valantinas .

Ethics declarations

Competing interests.

The authors declare no competing interests.

Peer review

Peer review information.

Nature Geoscience thanks Daniel Viudez-Moreiras and Aditya Khuller for their contribution to the peer review of this work. Primary Handling Editor: Tamara Goldin, in collaboration with the Nature Geoscience team.

Additional information

Publisher’s note Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Extended data

Extended data fig. 1 diurnal variations of frost halo on olympus mons..

HRSC images of Olympus Mons (lat = 18.2°N, lon = −133.2°E) acquired at different local times in MY 36. ( a, b ) Late morning images showing no evidence of frost on the bright halo deposit surrounding the volcano caldera. ( c, d ) Early morning images revealing the presence of frost on the bright halo deposit. The bright halo deposit is likely composed of fine-grained dust with low thermal conductivity, which facilitates frost formation. North is up in all panels. HRSC image IDs: hn705_0000 (a), hn772_0000 ( b ), hn889_0000 ( c ), hn948_0000 ( d ). Credit: ESA/DLR/FU Berlin.

Extended Data Fig. 2 Irregular frost distribution on the outskirts of Olympus Mons caldera.

( a ) Bright halo visible in the CTX global mosaic (Dickson et al., 2018). The bright halo deposit is also visible in HRSC non-detections in Extended Data Fig. 1 . ( b ) Dark windstreak and triangular bright unremoved dust deposits seen in CTX. ( c ) CaSSIS morning observation of froststreaks (lat/lon = 18.28°N, −134.24°E) that correlate with bright dust deposits seen in CTX. ( d, e ) Frost deposits leeward of small craters (lat/lon: 18.27°N, −134.24°E and 18.83°N, −133.65°E respectively). ( f, g ) Froststreaks that are parallel to local winds (lat/lon: 18.90°N, −133.65°E and 18.9°N −133.74°E respectively). ( h, i ) Small frost deposits on the rim of a collapse pit (lat/lon: 18.95°N, −133.69°E) and on the levee of a lava channel (lat/lon: 19.00°N, −133.71°E). North is up in all panels. CaSSIS IDs: MY37_023825_162_0 (LST =7:13AM; Ls = 42.84; c,d) and MY36_015229_160_0 (LST = 6:57AM; Ls = 35.24 ; e-i). Credit: a , b , NASA/JPL/MSSS/The Murray Lab; c – l , ESA/TGO/CaSSIS under a Creative Commons license CC-BY-SA 3.0 IGO .

Extended Data Fig. 3 CaSSIS frost detections in the Tharsis volcanic region.

Frost was detected only on and around the calderas of the three largest volcanoes such as Olympus, Arsia and Ascraeus Montes, but also on the smaller Ceraunius Tholus volcano. Frost has not been observed yet on Pavonis Mons and other Tharsis volcanoes. The basemap is the color hillshade MOLA data at 64 pixels per degree resolution. Credit: NASA/JPL/GSFC.

Extended Data Fig. 4 Frost on the caldera floor of Ceraunius Tholus volcano.

( a ) Wide angle view of Ceraunius Tholus (lat = 24.0°N, lon = −97.1°E) with CaSSIS early morning observation overlain on the CTX mosaic. ( b ) Zoomed in view of (a). White rectangle marks the close up in (c). ( c ) Ubiquitous frost coverage on the caldera floor and the apparent absence of frost on the caldera rim. ( d ) CaSSIS color NPB image of the Ceraunius Tholus caldera acquired at a different local time featuring no frost. Both CaSSIS images in (b) and (d) are acquired at similar incidence (and phase) angles, which suggests that photometric effects are not the cause of surface blueing. North is up in all panels. CaSSIS image IDs in order: MY37_023134_024_3_NPB ( a−c ) and MY36_022599_024_0_NPB ( d ). a , b , d , NASA/JPL/MSSS/The Murray Lab; a , b , c , d , ESA/TGO/CaSSIS under a Creative Commons license CC-BY-SA 3.0 IGO .

Extended Data Fig. 5 Greyscale CaSSIS filter images of a small crater presented in Fig. 2 .

( a–c ) Three individual filters: NIR (860–1100 nm), PAN (550–800 nm) and BLU (390–570 nm). ( d ) CaSSIS DEM of the same scene with the location of the spectral profile and the frost-free ROI used in the reflectance ratio ( Methods ) overlaid. The frost deposits are brighter and visible in the CaSSIS BLU filter. North is up in all panels. CaSSIS ID: MY35_008465_192_0 ( a − c ) and DEM ID: CAS-DTM-MY36_020366_190_1-OPD-03–01 ( d ). Credit: ESA/TGO/CaSSIS under a Creative Commons license CC-BY-SA 3.0 IGO .

Extended Data Fig. 6 Seasonal and local time coverage of CaSSIS early morning observations of Olympus Mons and Arsia Mons.

CaSSIS image coverage over Olympus Mons ( a ) and Arsia Mons ( b ). Based on these observations frost is not detected during late morning hours in Olympus Mons and around southern summer solstice (Ls ~270°) in Arsia Mons. The shaded grey region shows the CaSSIS observational bias (from 90 − 85° solar incidence) due to the low signal-to-noise ratio. Most observations were discarded in this region due to spectral ambiguity. The black lines mark the local sunrise time.

Extended Data Fig. 7 Microclimatic conditions simulated over Arsia Mons.

This figure illustrates the impact of Arsia Mons′ topography on localized atmospheric conditions (at 8AM, Ls = 90°, Fig. 2a ), depicted through ( a ) elevation gradients, ( b ) surface atmospheric pressure, ( c ) near-surface horizontal wind patterns, and ( d ) the temperature differential between the Martian surface and the local CO 2 frost point. The complex caldera topography of Arsia Mons is shown to substantially influence local pressure distributions, wind velocities, and thermal gradients. Notably, surface temperatures at sites identified by CaSSIS for frost presence exceed the CO 2 frost point by approximately 60 K, suggesting the predominance of H 2 O ice in these frost deposits.

Extended Data Fig. 8 Triangular (ternary) diagrams of boulder shape across six sites of interest.

Boulder shape and size analysis for Olympus Mons ( a , b ), Arsia Mons ( c ), Tharsis Tholus ( d ), Jovis Tholus ( e ), and Ulysses Tholus ( f ). The slope aspect of each site is indicated on the respective panel. The Olympus Mons ( a , b ) and Arsia Mons ( c ) sites were found to feature a distinct early morning frost signature (positives, blue), the other three sites not (negatives, red)( d – f ) – yet there is no obvious difference in boulder shape across those sites (the colored polygons underline the distribution of points). C = compact, P = platy, B = bladed, E = elongated, V = very; a = longest boulder dimension, b = intermediate boulder dimension, c = smallest boulder dimension. HiRISE image IDs ( a – f ): ESP_014275_1990_RED, ESP_043272_1980_RED, ESP_047439_1990_RED, PSP_009884_1980_RED, ESP_057843_1715_RED, ESP_012612_1940_RED, ESP_033711_1985_RED, and ESP_045619_1835_RED.

Supplementary information

Supplementary information.

Supplementary Figs. 1–13 and Text.

Supplementary Table 1

Additional CaSSIS observation details and GCM estimated surface temperatures.

Rights and permissions

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/ .

Reprints and permissions

About this article

Cite this article.

Valantinas, A., Thomas, N., Pommerol, A. et al. Evidence for transient morning water frost deposits on the Tharsis volcanoes of Mars. Nat. Geosci. (2024). https://doi.org/10.1038/s41561-024-01457-7

Download citation

Received : 01 June 2023

Accepted : 16 April 2024

Published : 10 June 2024

DOI : https://doi.org/10.1038/s41561-024-01457-7

Share this article

Anyone you share the following link with will be able to read this content:

Sorry, a shareable link is not currently available for this article.

Provided by the Springer Nature SharedIt content-sharing initiative

Quick links

• Explore articles by subject
• Guide to authors
• Editorial policies

Sign up for the Nature Briefing: Anthropocene newsletter — what matters in anthropocene research, free to your inbox weekly.

Space Team Europe for Ariane 6: Laëlla Marimoutou

• MP4 [19.88 MB]
• SOURCE MP4 [336.13 MB]

Thank you for liking

You have already liked this page, you can only like it once!

They say it takes a village to raise a child. To launch a rocket, we have the combined expertise and passion of Space Team Europe. Laëlla Marimoutou is one of many making the first Ariane 6 launch possible and has been interviewed as part of a series highlighting some of the people that make up this dream team.

ArianeGroup’s Laëlla Marimoutou works on quality assurance for Ariane 6. As Launch System Quality Assurance Deputy Laëlla ensures the rocket is ready for liftoff. Improvement is infinite and quality is inspiring.

Stay tuned for more from #SpaceTeamEurope: an ESA space community engagement initiative to gather European space actors under the same umbrella sharing values of leadership, autonomy, and responsibility.

Find more videos from Space Team Europe .

• CREDIT ESA - European Space Agency
• LICENCE ESA Standard Licence
• Closed captions available Captions and subtitles are available (automatically generated by YouTube) - select your language using the YouTube player controls. A non-YouTube version is available using the 'download' and 'source' buttons below.
• Documentary
• Space Transportation
• Centre Spatial Guyanais (CSG) French Guiana Kourou
• Launcher Launchers and space vehicles
• Space Team Europe

Ariane 6 team after combined tests

Wafaa with Ariane 6 test model on the launch pad

Wafaa during Ariane 6 upper part transfer

Wafaa with Ariane 5 launch VA253

Ariane 6 core stage assembling at CSG