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Devil’s in Details in Selfie Taken by NASA’s Mars Perseverance Rover
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Explore This Section Perseverance Home Mission Overview Rover Components Mars Rock Samples Where is Perseverance? Ingenuity Mars Helicopter Mission Updates Science Overview Objectives Instruments Highlights Exploration Goals News and Features Multimedia Perseverance Raw Images Images Videos Audio More Resources Mars Missions Mars Sample Return Mars Perseverance Rover Mars Curiosity Rover MAVEN Mars Reconnaissance Orbiter Mars Odyssey More Mars Missions Mars Home 3 min read
A Dust Devil Photobombs Perseverance!
Perseverance self portrait, acquired by the WATSON camera on Sol 1500 on Mars. The Bell Island borehole where the rover acquired a sample is visible in the workspace in front of the rover. NASA/JPL-Caltech/MSSS Written by Athanasios Klidaras, Ph.D. candidate at Purdue University, and Megan Kennedy Wu, Senior Mission Operations Specialist at Malin Space Science Systems
To celebrate her 1,500th Martian day (“Sol”) exploring the red planet, the Perseverance rover used its robotic arm to take a selfie of the rover and the surrounding landscape. But when team members reviewed the photo, they were surprised to find that Perseverance had been photobombed!
As the rover sat at the “Pine Pond” workspace, located on the outer rim of Jezero crater, which it has been exploring for the past several months, the Wide Angle Topographic Sensor for Operations and eNgineering (WATSON) camera on the end of its arm was used to acquire a 59-image mosaic of the rover. This is the fifth “selfie” that Perseverance has acquired since landing on Mars in 2021. The rover’s robotic arm is not visible in the self portrait because — just like a selfie you would take with your own cellphone camera — rover operators make sure not to have the arm get “in the way” of the body of the rover. This is even easier to do on Mars because Perseverance needs to take 59 different images at slightly different arm positions to build up the selfie, and the elbow of the robotic arm is kept out of the way while the images are acquired. You can find more details about the Sol 1500 selfie here, and this YouTube video shows how the rover arm moves when these activities take place.
While snapping away, Perseverance was photobombed by a dust devil in the distance! These are relatively common phenomena both on Mars and in Earth’s desert regions, and form from rising and rotating columns of warm air, which gives the appearance of a dust tornado. Just like many other weather patterns, there is a peak “season” for dust-devil activity, and Jezero crater is in the peak of that season now (late northern spring). The one seen in the selfie is fairly large, about 100 meters, or 328 feet, across. While Perseverance regularly monitors the horizon for dust-devil activity with Navcam movies, this is the first time the WATSON camera on the end of the robotic arm has ever captured an image of a dust devil!
The dark hole in front of the rover, surrounded by gray rock powder created during the drilling process, shows the location of Perseverance’s 26th sample. Nicknamed “Bell Island” after an island near Newfoundland, Canada, this rock sample contains small spherules, thought to have formed by volcanic eruptions or impacts early in Martian history. Later, this ancient rock was uplifted during the impact that formed Jezero crater. Now that the rover has successfully acquired the spherule sample the science team was searching for, Perseverance is leaving the area to explore new rock exposures. Last week, the rover arrived at an exposure of light-toned bedrock called “Copper Cove,” and the science team was interested to determine if this unit underlies or overlies the rock sequence explored earlier. After performing an abrasion to get a closer look at the chemistry and textures, the rover drove south to scout out more sites along the outer edge of the Jezero crater rim.
Learn more, and see more detailed views of Perseverance’s ‘Selfie With Dust Devil’
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Last Updated May 29, 2025 Related Terms
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After a decade of searching, NASA’s MAVEN (Mars Atmosphere Volatile Evolution) mission has, for the first time, reported a direct observation of an elusive atmospheric escape process called sputtering that could help answer longstanding questions about the history of water loss on Mars.
Scientists have known for a long time, through an abundance of evidence, that water was present on Mars’ surface billions of years ago, but are still asking the crucial question, “Where did the water go and why?”
Early on in Mars’ history, the atmosphere of the Red Planet lost its magnetic field, and its atmosphere became directly exposed to the solar wind and solar storms. As the atmosphere began to erode, liquid water was no longer stable on the surface, so much of it escaped to space. But how did this once thick atmosphere get stripped away? Sputtering could explain it.
Sputtering is an atmospheric escape process in which atoms are knocked out of the atmosphere by energetic charge particles.
“It’s like doing a cannonball in a pool,” said Shannon Curry, principal investigator of MAVEN at the Laboratory for Atmospheric and Space Physics at the University of Colorado Boulder and lead author of the study. “The cannonball, in this case, is the heavy ions crashing into the atmosphere really fast and splashing neutral atoms and molecules out.”
While scientists had previously found traces of evidence that this process was happening, they had never observed the process directly. The previous evidence came from looking at lighter and heavier isotopes of argon in the upper atmosphere of Mars. Lighter isotopes sit higher in the atmosphere than their heavier counterparts, and it was found that there were far fewer lighter isotopes than heavy argon isotopes in the Martian atmosphere. These lighter isotopes can only be removed by sputtering.
“It is like we found the ashes from a campfire,” said Curry. “But we wanted to see the actual fire, in this case sputtering, directly.”
To observe sputtering, the team needed simultaneous measurements in the right place at the right time from three instruments aboard the MAVEN spacecraft: the Solar Wind Ion Analyzer, the Magnetometer, and the Neutral Gas and Ion Mass Spectrometer. Additionally, the team needed measurements across the dayside and the nightside of the planet at low altitudes, which takes years to observe.
The combination of data from these instruments allowed scientists to make a new kind of map of sputtered argon in relation to the solar wind. This map revealed the presence of argon at high altitudes in the exact locations that the energetic particles crashed into the atmosphere and splashed out argon, showing sputtering in real time. The researchers also found that this process is happening at a rate four times higher than previously predicted and that this rate increases during solar storms.
The direct observation of sputtering confirms that the process was a primary source of atmospheric loss in Mars’ early history when the Sun’s activity was much stronger.
“These results establish sputtering’s role in the loss of Mars’ atmosphere and in determining the history of water on Mars,” said Curry.
The finding, published this week in Science Advances, is critical to scientists’ understanding of the conditions that allowed liquid water to exist on the Martian surface, and the implications that it has for habitability billions of years ago.
The MAVEN mission is part of NASA’s Mars Exploration Program portfolio. MAVEN’s principal investigator is based at the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado Boulder, which is also responsible for managing science operations and public outreach and communications. NASA’s Goddard Space Flight Center in Greenbelt, Maryland, manages the MAVEN mission. Lockheed Martin Space built the spacecraft and is responsible for mission operations. NASA’s Jet Propulsion Laboratory in Southern California provides navigation and Deep Space Network support.
More information on NASA’s MAVEN mission
By Willow Reed
Laboratory for Atmospheric and Space Physics, University of Colorado Boulder
Media Contacts:
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NASA’s Goddard Space Flight Center, Greenbelt, Md.
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Last Updated May 28, 2025 Related Terms
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Preparations for Next Moonwalk Simulations Underway (and Underwater)
Artist concept highlighting the novel approach proposed by the 2025 NIAC awarded selection of MaRS ICICLE concept.NASA/Aaswath Pattabhi Raman Aaswath Pattabhi Raman
University of California, Los Angeles
Exploration of Mars has captivated the public in recent decades with high-profile robotic missions and the images they have acquired seeding our collective imagination. NASA is actively planning for human exploration of Mars and laid out some of the key capabilities that must be developed to execute successful, cost-effective programs that would put human beings on the surface of another planet and bring them home safely. Efficient, flexible and productive round-trip missions will be key to further human exploration of Mars. New round-trip mission concepts however need substantially improved long-duration storage of cryogenic propellants in various space environments; relevant propellants include liquid Hydrogen (LH2) for high specific impulse Nuclear Thermal Propulsion (NTP) which can be deployed in strategic locations in advance of a mission. If enabled, such LH2 storage tanks could be used to refill a crewed Mars Transfer Vehicle (MTV) to send and bring astronauts home quickly, safely, and cost-effectively. A well-designed cryogenic propellant storage tank can reflect the vast majority of photons incident on the spacecraft, but not all. In thermal environments like Low Earth Orbit (LEO), there is residual heating due to light directly from the Sun, sunlight reflected off Earth, and blackbody thermal radiation from Earth. Over time, this leads to some of the propellant molecules absorbing the requisite latent heat of vaporization, entering the gas phase, and ultimately being released into space to prevent an unsustainable build-up of pressure in the tank. This slow “boil-off” process leads to significant losses of the cryogenic liquid into space, potentially leaving it with insufficient mass and greatly limiting Mars missions. We propose a breakthrough mission concept: an ultra-efficient round-trip Mars mission with zero boil off of propellants. This will be enabled by low-cost, efficient cryogenic liquid storage capable of storing LH2 and LOx with ZBO even in the severe and fluctuating thermal environment of LEO. To enable this capability, the propellant tanks in our mission will employs thin, lightweight, all-solid-state panels attached to the tank’s deep-space-facing surfaces that utilize a long-understood but as-yet-unrealized cooling technology known as Electro-Luminescent Cooling (ELC) to reject heat from cold solid surfaces as non-equilibrium thermal radiation with significantly more power density than Planck’s Law permits for equilibrium thermal radiation. Such a propellant tank would drastically lower the cost and complexity of propulsion systems for crewed Mars missions and other deep space exploration by allowing spacecraft to refill propellant tanks after reaching orbit rather than launching on the much larger rocket required to lift the spacecraft in a single-use stage. To achieve ZBO, a storage spacecraft must keep the storage tank’s temperature below the boiling point of the cryogen (e.g., < 90 K for LOx and < 20 K for liquid H2). Achieving this in LEO-like thermal environments requires both excellent reflectivity toward sunlight and thermal radiation from the Earth, Mars and other nearby bodies as well as a power-efficient cooling mechanism to remove what little heat inevitably does leak in, a pair of conditions ideally suited to the ELC cooling systems that will makes our full return-trip mission to Mars a success.
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Last Updated May 27, 2025 EditorLoura Hall Related Terms
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Preparations for Next Moonwalk Simulations Underway (and Underwater)
One of the navigation cameras on NASA’s Perseverance captured the rover’s tracks coming from an area called “Witch Hazel Hill,” on May 13, 2025, the 1,503rd Martian day, or sol, of the mission. NASA/JPL-Caltech Scientists expect the new area of interest on the lower slope of Jezero Crater’s rim to offer up some of the oldest rocks on the Red Planet.
NASA’s Perseverance Mars rover is exploring a new region of interest the team is calling “Krokodillen” that may contain some of the oldest rocks on Mars. The area has been on the Perseverance science team’s wish list because it marks an important boundary between the oldest rocks of Jezero Crater’s rim and those of the plains beyond the crater.
“The last five months have been a geologic whirlwind,” said Ken Farley, deputy project scientist for Perseverance from Caltech in Pasadena. “As successful as our exploration of “Witch Hazel Hill” has been, our investigation of Krokodillen promises to be just as compelling.”
Named by Perseverance mission scientists after a mountain ridge on the island of Prins Karls Forland, Norway, Krokodillen (which means “the crocodile” in Norwegian) is a 73-acre (about 30-hectare) plateau of rocky outcrops located downslope to the west and south of Witch Hazel Hill.
A quick earlier investigation into the region revealed the presence of clays in this ancient bedrock. Because clays require liquid water to form, they provide important clues about the environment and habitability of early Mars. The detection of clays elsewhere within the Krokodillen region would reinforce the idea that abundant liquid water was present sometime in the distant past, likely before Jezero Crater was formed by the impact of an asteroid. Clay minerals are also known on Earth for preserving organic compounds, the building blocks of life.
“If we find a potential biosignature here, it would most likely be from an entirely different and much earlier epoch of Mars evolution than the one we found last year in the crater with ‘Cheyava Falls,’” said Farley, referring to a rock sampled in July 2024 with chemical signatures and structures that could have been formed by life long ago. “The Krokodillen rocks formed before Jezero Crater was created, during Mars’ earliest geologic period, the Noachian, and are among the oldest rocks on Mars
Data collected from NASA’s Mars orbiters suggest that the outer edges of Krokodillen may also have areas rich in olivine and carbonate. While olivine forms from magma, carbonate minerals on Earth typically form during a reaction in liquid water between rock and dissolved carbon dioxide. Carbonate minerals on Earth are known to be excellent preservers of fossilized ancient microbial life and recorders of ancient climate.
The rover, which celebrated its 1,500th day of surface operations on May 9, is currently analyzing a rocky outcrop in Krokodillen called “Copper Cove” that may contain Noachian rocks.
Ranking Mars Rocks
The rover’s arrival at Krokodillen comes with a new sampling strategy for the nuclear-powered rover that allows for leaving some cored samples unsealed in case the mission finds a more scientifically compelling geologic feature down the road.
To date, Perseverance has collected and sealed two regolith (crushed rock and dust) samples, three witness tubes, and one atmospheric sample. It has also collected 26 rock cores and sealed 25 of them. The rover’s one unsealed sample is its most recent, a rock core taken on April 28 that the team named “Bell Island,” which contains small round stones called spherules. If at some point the science team decides a new sample should take its place, the rover could be commanded to remove the tube from its bin in storage and dump the previous sample.
“We have been exploring Mars for over four years, and every single filled sample tube we have on board has its own unique and compelling story to tell,” said Perseverance acting project scientist Katie Stack Morgan of NASA’s Jet Propulsion Laboratory in Southern California. “There are seven empty sample tubes remaining and a lot of open road in front of us, so we’re going to keep a few tubes — including the one containing the Bell Island core — unsealed for now. This strategy allows us maximum flexibility as we continue our collection of diverse and compelling rock samples.”
Before the mission adopted its new strategy, the engineering sample team assessed whether leaving a tube unsealed could diminish the quality of a sample. The answer was no.
“The environment inside the rover met very strict standards for cleanliness when the rover was built. The tube is also oriented in such a way within its individual storage bin that the likelihood of extraneous material entering the tube during future activities, including sampling and drives, is very low,” said Stack Morgan.
In addition, the team assessed whether remnants of a sample that was dumped could “contaminate” a later sample. “Although there is a chance that any material remaining in the tube from the previous sample could come in contact with the outside of a new sample,” said Stack Morgan, “it is a very minor concern — and a worthwhile exchange for the opportunity to collect the best and most compelling samples when we find them.”
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Jet Propulsion Laboratory, Pasadena, Calif.
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NASA Headquarters, Washington
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Last Updated May 19, 2025 Related Terms
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