¹S.A.Connell et al. (>10)
Journal of Geophysical Research (Planets)(in Press) Open Access Link to Article [https://doi.org/10.1029/2025JE009243]
¹Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA
Published by arrangement with John Wiley & Sons

Investigating the stability of hydrated minerals is integral for examining the preservation ofrocks for potential Mars Sample Return and has major implications for models that use rover‐basedobservations to quantify Mars’ global water budget. The Mars 2020 Perseverance rover produces abrasionpatches to investigate fresh rock surfaces at Jezero crater, Mars. However, due to operational constraints, thefull analysis process typically takes several martian days (sols), and freshly exposed hydrated minerals maydehydrate upon atmospheric exposure between abrasion patch creation and their analyses. To assess thepotential for short‐term dehydration, the SuperCam instrument conducted the first in situ rover‐based dehydration experiment on rock exposures of the “Bright Angel formation.” The SuperCam andSHERLOC rover instruments indicated that the primary mineral hydration phases were Fe‐hydroxides, Ca‐sulfates such as bassanite (mixed with anhydrite), with possible minor contributions from non‐interlayer‐waterphyllosilicates (e.g., hydroxyl‐bearing only). The experiment involved a four‐sol sequence of observations onthe Steamboat Mountain abrasion patch, beginning just 22 min after abrasion. Dehydration was assessed bytracking changes in the 1.93 μm H2O absorption feature, which is sensitive to structural, absorbed, andadsorbed water. No significant changes in hydration were observed over the 93 hr, suggesting that the exposedminerals were already in a low hydration state and/or exhibit high stability under current martian surfaceconditions. These findings imply bulk rocks with low hydration and high stability minerals may not dehydrateupon exposure to the modern martian atmosphere on short time scales, consistent with predictions fromlaboratory simulations of Mars‐like environments.

^1,2Angel Mojarro,²José C. Aponte,²Jason P. Dworkin,²Jamie E. Elsila,²Daniel P. Glavin^3,4,5, Harold C. Connolly Jr.,³Dante S. Lauretta
Proceedings of the Nstional Academy of Sciences of the USA (in Press) Open Access Link to Article [https://doi.org/10.1073/pnas.25124611]
¹National Aeronautics and Space Administration Postdoctoral Program, Oak Ridge Associated Universities, Oak Ridge, TN 37830
²Solar System Exploration Division, National Aeronautics and Space Administration, Goddard Space Flight Center, Greenbelt, MD 20771
³Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721
⁴Department of Geology, School of Earth and Environment, Rowan University, Glassboro, NJ 08028
⁵Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024

NASA’s OSIRIS-REx mission characterized the asteroid Bennu and delivered pristine samples of its regolith to Earth. Coordinated analyses of this primitive, carbonaceous material are elucidating the abiotic formation and inventory of prebiotic organic compounds in the early Solar System. Using pyrolysis and wet-chemistry techniques, we analyzed aggregate (unsorted particulate) material and three distinct stones that appear to correspond to different boulder types observed by the spacecraft. Results from the aggregate were consistent with previous work that detected the five canonical nucleobases and 14 of the 20 α-amino acids utilized by life to synthesize proteins. However, our analytical approach tentatively uncovered trace signals of a fifteenth α-amino acid, tryptophan, which has not been detected previously in extraterrestrial materials. Further, we found that the distributions of insoluble and soluble-derived organics differ between distinct stones, suggesting heterogeneous geologic processing within Bennu’s parent body. The distributions of alkylated polycyclic aromatic hydrocarbons resemble those in aqueously altered carbonaceous chondrites and are consistent with an abiotic origin through aqueous reactions. Our findings expand the evidence that prebiotic organic molecules can form within primitive accreting planetary bodies and could have been delivered via impacts to the early Earth and other Solar System bodies, potentially contributing to the origins of life.