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Mars: Perseverance (Mars 2020) 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 The Solar System The Sun Mercury Venus Earth The Moon Mars Jupiter Saturn Uranus Neptune Pluto & Dwarf Planets Asteroids, Comets & Meteors The Kuiper Belt The Oort Cloud 3 min read
Behind the Scenes at the 2024 Mars 2020 Science Team Meeting
The Mars 2020 Perseverance Rover Science Team meets in person and online during the July 2024 team meeting in Pasadena, CA. Credits: R. Hogg and J. Maki. The Mars 2020 Science Team meets in Pasadena for 3 days of science synthesis
It has become a fun tradition for me to write a summary of our yearly in-person Science Team Meetings (2022 meeting and 2023 meeting). I’ve been particularly looking forward to this year’s update given the recent excitement on the team and in the public about Perseverance’s discovery of a potential biosignature, a feature that may have a biological origin but needs more data or further study before reaching a conclusion about the absence or presence of life.
This past July, ~160 members of the Mars 2020 Science Team met in-person in Pasadena—with another ~50 team members dialed in on-line—for three days of presentations, meetings, and team discussion. For a team that spends most of the year working remotely from around the world, we make the most of these rare opportunities for in-person discussion and synthesis of the rover’s latest science results.
We spent time discussing Perseverance’s most recent science campaign in the Margin unit, an exposure of carbonate-bearing rocks that occurs along the inner rim of Jezero crater. As part of an effort to synthesize what we’ve learned about the Margin unit over the past year, we heard presentations describing surface and subsurface observations collected from the rover’s entire payload. This was followed by a thought-provoking series of presentations that tackled the three hypotheses we’re carrying for the origin of this unit: sedimentary, volcanic (pyroclastic), or crystalline igneous.
Some of our liveliest discussion occurred during presentations about Neretva Vallis, Jezero’s inlet valley that once fed the sedimentary fan and lake system within the crater. Data from the RIMFAX instrument took center stage as we debated the origin and age relationship of the Bright Angel outcrop to other units we’ve studied in the crater.
This context is especially important because the Bright Angel outcrop is home to the Cheyava Falls rock, which contains intriguing features we’ve been calling “leopard spots,” small white spots with dark rims observed in red bedrock of Bright Angel. On the last day of the team meeting, data from our recent “Apollo Temple” abrasion at Cheyava Falls was just starting to arrive on Earth, and team members from the PIXL and SHERLOC teams were huddled in the hallway and at the back of the conference room trying to digest these new results in real time. We had special “pop-up” presentations during which SHERLOC reported compelling evidence for organics in the new abrasion, and PIXL showed interesting new data about the light-toned veins that crosscut this rock.
Between debates about the Margin unit, updates on recently published studies of the Jezero sedimentary fan sequence, and discussion of the newest rocks at Bright Angel, this team meeting was one of our most exciting yet. It also marked an important transition for the Mars 2020 science mission as we prepare to ascend the Jezero crater rim, leaving behind—at least for now—the rocks inside the crater. I can only imagine the interesting new discoveries we’ll make during the upcoming year, and I can’t wait to report back next summer!
Written by Katie Stack Morgan, Mars 2020 Deputy Project Scientist at NASA’s Jet Propulsion Laboratory
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Last Updated Aug 30, 2024 Related Terms
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NASA, ESA Missions Help Scientists Uncover How Solar Wind Gets Energy
Since the 1960s, astronomers have wondered how the Sun’s supersonic “solar wind,” a stream of energetic particles that flows out into the solar system, continues to receive energy once it leaves the Sun. Now, thanks to a lucky lineup of a NASA and an ESA (European Space Agency)/NASA spacecraft both currently studying the Sun, they may have discovered the answer — knowledge that is a crucial piece of the puzzle to help scientists better forecast solar activity between the Sun and Earth.
A paper published in the Aug. 30, 2024, issue of the journal Science provides persuasive evidence that the fastest solar winds are powered by magnetic “switchbacks,” or large kinks in the magnetic field, near the Sun.
“Our study addresses a huge open question about how the solar wind is energized and helps us understand how the Sun affects its environment and, ultimately, the Earth,” said Yeimy Rivera, co-leader of the study and a postdoctoral fellow at the Smithsonian Astrophysical Observatory, part of Center for Astrophysics | Harvard & Smithsonian. “If this process happens in our local star, it’s highly likely that this powers winds from other stars across the Milky Way galaxy and beyond and could have implications for the habitability of exoplanets.”
This artist’s concept shows switchbacks, or large kinks in the Sun’s magnetic field. NASA’s Goddard Space Flight Center/Conceptual Image Lab/Adriana Manrique Gutierrez Previously, NASA’s Parker Solar Probe found that these switchbacks were common throughout the solar wind. Parker, which became the first craft to enter the Sun’s magnetic atmosphere in 2021, allowed scientists to determine that switchbacks become more distinct and more powerful close to the Sun. Up to now, however, scientists lacked experimental evidence that this interesting phenomenon actually deposits enough energy to be important in the solar wind.
“About three years ago, I was giving a talk about how fascinating these waves are,” said co-author Mike Stevens, astrophysicist at the Center for Astrophysics. “At the end, an astronomy professor stood up and said, ‘that’s neat, but do they actually matter?’”
To answer this, the team of scientists had to use two different spacecraft. Parker is built to fly through the Sun’s atmosphere, or “corona.” ESA’s and NASA’s Solar Orbiter mission is also on an orbit that takes it relatively close to the Sun, and it measures solar wind at larger distances.
The discovery was made possible because of a coincidental alignment in February 2022 that allowed both Parker Solar Probe and Solar Orbiter to measure the same solar wind stream within two days of each other. Solar Orbiter was almost halfway to the Sun while Parker was skirting the edge of the Sun’s magnetic atmosphere.
This conceptual image shows Parker Solar Probe about to enter the solar corona. NASA/Johns Hopkins APL/Ben Smith An artist’s concept shows Solar Orbiter near the Sun. NASA’s Goddard Space Flight Center Conceptual Image Lab
“We didn’t initially realize that Parker and Solar Orbiter were measuring the same thing at all. Parker saw this slower plasma near the Sun that was full of switchback waves, and then Solar Orbiter recorded a fast stream which had received heat and with very little wave activity,” said Samuel Badman, astrophysicist at the Center for Astrophysics and the other co-lead of the study. “When we connected the two, that was a real eureka moment.”
Scientists have long known that energy is moved throughout the Sun‘s corona and the solar wind, at least in part, through what are known as “Alfvén waves.” These waves transport energy through a plasma, the superheated state of matter that makes up the solar wind.
However, how much the Alfvén waves evolve and interact with the solar wind between the Sun and Earth couldn’t be measured — until these two missions were sent closer to the Sun than ever before, at the same time. Now, scientists can directly determine how much energy is stored in the magnetic and velocity fluctuations of these waves near the corona, and how much less energy is carried by the waves farther from the Sun.
The new research shows that the Alfvén waves in the form of switchbacks provide enough energy to account for the heating and acceleration documented in the faster stream of the solar wind as it flows away from the Sun.
“It took over half a century to confirm that Alfvenic wave acceleration and heating are important processes, and they happen in approximately the way we think they do,” said John Belcher, emeritus professor from the Massachusetts Institute of Technology who co-discovered Alfvén waves in the solar wind but was not involved in this study.
In addition to helping scientists better forecast solar activity and space weather, such information helps us understand mysteries of the universe elsewhere and how Sun-like stars and stellar winds operate everywhere.
“This discovery is one of the key puzzle pieces to answer the 50-year-old question of how the solar wind is accelerated and heated in the innermost portions of the heliosphere, bringing us closer to closure to one of the main science objectives of the Parker Solar Probe mission,” said Adam Szabo, Parker Solar Probe mission science lead at NASA.
By Megan Watzke
Center for Astrophysics | Harvard & Smithsonian
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Last Updated Aug 30, 2024 Related Terms
Goddard Space Flight Center Heliophysics Heliophysics Division Parker Solar Probe (PSP) Science & Research Science Mission Directorate Solar Flares Solar Orbiter Solar Science Solar Wind Space Weather The Sun The Sun & Solar Physics Explore More
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