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153. The Propitious Role of Solar Energetic Particles in the Origin of Life

Author

Lingam, Manasvi, Dong, Chuanfei, Fang, Xiaohua, Jakosky, Bruce M., Loeb, Abraham, Lingam, Manasvi, Dong, Chuanfei, Fang, Xiaohua, Jakosky, Bruce M., and Loeb, Abraham

Abstract

We carry out 3-D numerical simulations to assess the penetration and bombardment effects of Solar Energetic Particles (SEPs), i.e. high-energy particle bursts during large flares and superflares, on ancient and current Mars. We demonstrate that the deposition of SEPs is non-uniform at the planetary surface, and that the corresponding energy flux is lower than other sources postulated to have influenced the origin of life. Nevertheless, SEPs may have been capable of facilitating the synthesis of a wide range of vital organic molecules (e.g. nucleobases and amino acids). Owing to the relatively high efficiency of these pathways, the overall yields might be comparable to (or even exceed) the values predicted for some conventional sources such as electrical discharges and exogenous delivery by meteorites. We also suggest that SEPs could have played a role in enabling the initiation of lightning. A notable corollary of our work is that SEPs may constitute an important mechanism for prebiotic synthesis on exoplanets around M-dwarfs, thereby mitigating the deficiency of biologically active ultraviolet radiation on these planets. Although there are several uncertainties associated with (exo)planetary environments and prebiotic chemical pathways, our study illustrates that SEPs represent a potentially important factor in understanding the origin of life., Comment: published in The Astrophysical Journal; 14 pages; 2 figures

Published
2018
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154. Superthermal Electron Deposition on the Mars Nightside During ICMEs.

Author

Xu, Shaosui, Curry, Shannon M., Mitchell, David L., Luhmann, Janet G., Lillis, Robert J., and Dong, Chuanfei

Subjects
GEOMAGNETISM, MAGNETOSPHERE, MAGNETIC storms, SOLAR wind, IONOSPHERE
Abstract

Superthermal electron precipitation is one of the main sources supporting the Mars nightside ionosphere. It is expected that solar wind electron fluxes are to increase significantly during interplanetary coronal mass ejections (ICMEs) and therefore an enhanced nightside ionospheric density. This study is to quantify the variation of the precipitating and deposited electron fluxes during five extreme ICMEs encountered by Mars Global Surveyor (MGS). We find that energy fluxes correlate better with the upstream dynamic pressure proxy than number fluxes and electron fluxes increase more at high energies, which means that electrons tend to have a lower peak production altitude during storm times. The precipitating and net/deposited fluxes are increased up to an order of magnitude from low to high dynamic pressures. The estimated total electron content (TEC) is a few times of 1014 m−2 for quiet times and on the order of 1015 m−2 for storm times, with an enhancement up to an order of magnitude locally near strong crustal fields. Crustal magnetic fields have an effect on the deposited fluxes with more prominent magnetic reflection over strong magnetic fields during quiet periods, which is significantly reduced during storm times. Lastly, we estimate a global energy input from downward fluxes of 1.1 × 108 and 5.5 × 108 W and the globally deposited energy from net fluxes of 2.0 × 107 and 1.6 × 108 W for quiet and storm time periods, a factor of 5 and 8 enhancement globally, respectively, but up to an order of magnitude locally near strong crustal fields. Key Points: We quantify the variation of nightside precipitating and deposited electron fluxes during five extreme ICME events encountered by MGSThe estimated TEC is on the order of 1014 m−2 for quiet periods and 1015 m−2 for storm periods because of enhanced electron precipitationCrustal magnetic fields reduce deposited fluxes during quiet time because of magnetic reflection, which is largely reduced during storm time [ABSTRACT FROM AUTHOR]

Published
2020
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157. The Impact and Solar Wind Proxy of the 2017 September ICME Event at Mars

Author

Ma, Yingjuan, primary, Fang, Xiaohua, additional, Halekas, Jasper S., additional, Xu, Shaosui, additional, Russell, Christopher T., additional, Luhmann, Janet G., additional, Nagy, Andrew F., additional, Toth, Gabor, additional, Lee, Christina O., additional, Dong, Chuanfei, additional, Espley, Jared R., additional, McFadden, James P., additional, Mitchell, David L., additional, and Jakosky, Bruce M., additional

Published
2018
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158. Solar Wind Interaction With the Martian Upper Atmosphere: Roles of the Cold Thermosphere and Hot Oxygen Corona

Author

Dong, Chuanfei, primary, Bougher, Stephen W., additional, Ma, Yingjuan, additional, Lee, Yuni, additional, Toth, Gabor, additional, Nagy, Andrew F., additional, Fang, Xiaohua, additional, Luhmann, Janet, additional, Liemohn, Michael W., additional, Halekas, Jasper S., additional, Tenishev, Valeriy, additional, Pawlowski, David J., additional, and Combi, Michael R., additional

Published
2018
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160. Modeling Martian Atmospheric Losses over Time: Implications for Exoplanetary Climate Evolution and Habitability

Author

Dong, Chuanfei, primary, Lee, Yuni, additional, Ma, Yingjuan, additional, Lingam, Manasvi, additional, Bougher, Stephen, additional, Luhmann, Janet, additional, Curry, Shannon, additional, Toth, Gabor, additional, Nagy, Andrew, additional, Tenishev, Valeriy, additional, Fang, Xiaohua, additional, Mitchell, David, additional, Brain, David, additional, and Jakosky, Bruce, additional

Published
2018
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165. The dehydration of water worlds via atmospheric losses

Author

Dong, Chuanfei, Huang, Zhenguang, Lingam, Manasvi, Tóth, Gábor, Gombosi, Tamas, Bhattacharjee, Amitava, Dong, Chuanfei, Huang, Zhenguang, Lingam, Manasvi, Tóth, Gábor, Gombosi, Tamas, and Bhattacharjee, Amitava

Abstract

We present a three-species multi-fluid MHD model (H$^+$, H$_2$O$^+$ and e$^-$), endowed with the requisite atmospheric chemistry, that is capable of accurately quantifying the magnitude of water ion losses from exoplanets. We apply this model to a water world with Earth-like parameters orbiting a Sun-like star for three cases: (i) current normal solar wind conditions, (ii) ancient normal solar wind conditions, and (iii) one extreme "Carrington-type" space weather event. We demonstrate that the ion escape rate for (ii), with a value of 6.0$\times$10$^{26}$ s$^{-1}$, is about an order of magnitude higher than the corresponding value of 6.7$\times$10$^{25}$ s$^{-1}$ for (i). Studies of ion losses induced by space weather events, where the ion escape rates can reach $\sim$ 10$^{28}$ s$^{-1}$, are crucial for understanding how an active, early solar-type star (e.g., with frequent coronal mass ejections) could have accelerated the depletion of the exoplanet's atmosphere. We briefly explore the ramifications arising from the loss of water ions, especially for planets orbiting M-dwarfs where such effects are likely to be significant., Comment: ApJ Letters, in press, 8 pages, 2 figures, 3 tables

Published
2017
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166. MAVEN observations of atmospheric loss at Mars

Author

Curry, Shannon, Luhmann, Janet, Jakosky, Bruce M., Brain, David, Leblanc, Francis, Modolo, Ronan, Halekas, Jasper S., Schneider, Nicholas M., Deighan, Justin, Mcfadden, James, Espley, Jared R., Mitchell, David L., Connerney, J. E. P., Dong, Yaxue, Dong, Chuanfei, Ma, Yingjuan, Cohen, Ofer, Fränz, Markus, Holmström, Mats, Ramstad, Robin, Hara, Takuya, Lillis, Robert J., Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Département de physique et d'astronomie, Université de Moncton, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], NASA Goddard Space Flight Center (GSFC), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), Swedish Institute of Space Physics [Kiruna] (IRF), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)

Subjects
Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

International audience; The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission has been making observations of the Martian upper atmosphere and its escape to space since November 2014. The subject of atmospheric loss at terrestrial planets is a subject of intense interest not only because of the implications for past and present water reservoirs, but also for its impacts on the habitability of a planet. Atmospheric escape may have been especially effective at Mars, relative to Earth or Venus, due to its smaller size as well as the lack of a global dynamo magnetic field. Not only is the atmosphere less gravitationally bound, but also the lack of global magnetic field allows the impinging solar wind to interact directly with the Martian atmosphere. When the upper atmosphere is exposed to the solar wind, planetary neutrals can be ionized and 'picked up' by the solar wind and swept away.Both neutral and ion escape have played significant roles the long term climate change of Mars, and the MAVEN mission was designed to directly measure both escaping planetary neutrals and ions with high energy, mass, and time resolution. We will present 1.5 years of observations of atmospheric loss at Mars over a variety of solar and solar wind conditions, including extreme space weather events. We will report the average ion escape rate and the spatial distribution of escaping ions as measured by MAVEN and place them in context both with previous measurements of ion loss by other spacecraft (e.g. Phobos 2 and Mars Express) and with estimates of neutral escape rates by MAVEN. We will then report on the measured variability in ion escape rates with different drivers (e.g. solar EUV, solar wind pressure, etc.) and the implications for the total ion escape from Mars over time. Additionally, we will also discuss the implications for atmospheric escape at exoplanets, particularly weakly magnetized planetary bodies orbiting M-dwarfs, and the dominant escape mechanisms that may drive atmospheric erosion in other stellar systems.

Published
2016

171. The Loss Rate of Ions from the Martian Atmosphere

Author

Brain, Dave, Mcfadden, James, Halekas, Jasper, Connerney, John, Bougher, Stephen, Curry, Shannon, Dong, Chuanfei, Dong, Yaxue, Eparvier, Francis G., Fang, Xiaohua, Fortier, Kier, Hara, Takuya, Harada, Yuki, Jakosky, Bruce M., Lillis, Robert, Livi, Roberto, Luhmann, Janet G., Ma, Yingjuan, Modolo, Ronan, Seki, Kanako, Thiemann, Ed, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, University of Iowa [Iowa City], NASA Goddard Space Flight Center (GSFC), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, University of Michigan System, Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Nagoya University, University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)

Subjects
Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; In November 2014 the MAVEN (Mars Atmosphere and Volatile EvolutioN) spacecraft began the science phase of its mission to study the upper atmosphere of Mars and its escape to space. The loss of atmospheric particles (in neutral or charged state) to space is thought to have played a role in the evolution of the Martian climate over the past ~4 billion years. Charged particle escape at Mars may be significant due to the absence of a global dynamo magnetic field for most of its history, allowing more direct access of the solar wind to the Martian atmosphere. Among its many measurement capabilities, MAVEN can detect escaping planetary ions with high time cadence and high energy and mass resolution using the STATIC (SupraTheral and Thermal Ion Composition) instrument.We present the results of an effort to compute the escape rate of ions from the Martian atmosphere over MAVEN’s primary mission. We statistically map the measured fluxes of planetary ions to various surfaces near Mars, including a closed spherical shell surrounding the planet. We map both incoming and outgoing ion fluxes over different mass and energy ranges, and separate the fluxes by different drivers of escape measured by MAVEN, including solar wind pressure, Extreme Ultraviolet flux, and Interplanetary Magnetic Field strength. We place our results in context with measurements of ion escape made by the Phobos 2 and Mars Express missions, and address the implications for atmospheric loss over the history of the planet.

Published
2015

172. Consequences of simulated ion precipitation and sputtering during extreme conditions at Mars: comparison to MAVEN observations

Author

Curry, Shannon M., Luhmann, Janet, Dong, Chuanfei, Leblanc, François, Modolo, Ronan, Mcfadden, James, Ma, Yingjuan, Brain, Dave, Halekas, Jasper, Connerney, John, Espley, Jared, Harada, Yuki, Hara, Takuya, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Department of Physics and Astronomy [Ames, Iowa], Iowa State University (ISU), NASA Goddard Space Flight Center (GSFC), University of California [Berkeley], and University of California-University of California

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

International audience; Mars lacks an intrinsic dipole magnetic field, creating a scenario where the solar wind directly interacts with the upper atmosphere and newly created ions can be picked up and swept away by the background convection electric field. These pick-up ions can directly escape or precipitate back into the atmosphere and induce atmospheric sputtering of neutrals. Sputtering is believed to be one of the main drivers of atmospheric escape during the early epochs of our solar system when the solar activity and EUV intensities were much higher than the present day. Using the March 8th ICME event and other extreme solar wind events, we simulate three phases of the Mars-solar wind interaction using fluid and kinetic models and compare the predicted heavy ion precipitation with MAVEN observations in order to derive heavy ion precipitation and the first set of data-based sputtering rates. The fluid model reproduces the observed features in the solar wind density, velocity and magnetic field seen along the MAVEN orbit during the March 8th ICME event, and the subsequent precipitation shows strong agreement with other published predictions of sputtering in extreme conditions.

Published
2015

173. Mars Upper Atmospheric Responses to the 10 September 2017 Solar Flare: A Global, Time‐Dependent Simulation.

Author

Fang, Xiaohua, Pawlowski, David, Ma, Yingjuan, Bougher, Stephen, Thiemann, Edward, Eparvier, Francis, Wang, Wenbin, Dong, Chuanfei, Lee, Christina O., Dong, Yaxue, Benna, Mehdi, Elrod, Meredith, Chamberlin, Phillip, Mahaffy, Paul, and Jakosky, Bruce

Subjects
MARTIAN atmosphere, SOLAR flares, IONOSPHERIC electron density, MARS (Planet), UPPER atmosphere
Abstract

We report the first global, time‐dependent simulation of the Mars upper atmospheric responses to a realistic solar flare event, an X8.2 eruption on 10 September 2017. The Mars Global Ionosphere‐Thermosphere Model runs with realistically specified flare irradiance, giving results in reasonably good agreement with the Mars Atmosphere and Volatile EvolutioN spacecraft measurements. It is found that the ionized and neutral regimes of the upper atmosphere are significantly disturbed by the flare but react differently. The ionospheric electron density enhancement is concentrated below ∼110‐km altitude due to enhanced solar X‐rays, closely following the time evolution of the flare. The neutral atmospheric perturbation increases with altitude and is important above ∼150‐km altitude, in association with atmospheric upwelling driven by solar extreme ultraviolet heating. It takes ∼2.5 hr past the flare peak to reach the maximum disturbance and then additional ∼10 hr to generally settle down to preflare levels. Key Points: Ionospheric perturbation follows the flare in time and is concentrated mostly below 110‐km altitudeNeutral atmospheric perturbation increases with altitude and is important above 150‐km altitudeIt takes the neutral atmosphere 2.5 hr to reach the perturbation peak and 10 more hours to generally recover [ABSTRACT FROM AUTHOR]

Published
2019
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174. Magnetic Topology Response to the 2003 Halloween ICME Event at Mars.

Author

Xu, Shaosui, Curry, Shannon M., Mitchell, David L., Luhmann, Janet G., Lillis, Robert J., and Dong, Chuanfei

Subjects
CORONAL mass ejections, SPACE environment, MARTIAN atmosphere, INTERPLANETARY magnetic fields, MAGNETOHYDRODYNAMICS
Abstract

Understanding how the Mars plasma environment responds to space weather events provides insights into the early Sun‐Mars interaction and helps constrain the extrapolation of atmospheric loss back in time. The 2003 Halloween interplanetary coronal mass ejection (ICME) event is one of the most extreme space weather events encountered by Mars during the last two decades. Mars Global Surveyor's circular orbit at ∼400 km allows us to observationally study the magnetic topology response to this extreme event globally for the first time. We analyze the suprathermal electron data and magnetic field measurements from Mars Global Surveyor to infer magnetic topology before, during, and after this ICME event and quantify the variation of the topology over both weak and strong crustal regions and correlate the variation with the upstream dynamic pressure. Over weak crustal regions, more draped field lines and fewer closed field lines are observed under high dynamic pressures, implying a deeper interplanetary magnetic field penetration during the ICME event. Over dayside strong crustal regions, the dominant magnetic topology switches from closed field lines during quiet periods to open field lines during disturbed periods, suggesting more reconnection occurring between the crustal magnetic fields and interplanetary magnetic field. This mixed magnetic topological response is consistent with predictions from magnetohydrodynamic simulations for ICME events in previous studies. Key Points: We analyze Martian magnetic topology response to the 2003 Halloween ICME event and correlate the variation with upstream driversA deeper IMF penetration is found over weak crustal regions but more open field lines over strong crustal regions during the eventThis mixed magnetic topological response confirms previous predictions from MHD simulations for ICME events [ABSTRACT FROM AUTHOR]

Published
2019
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175. The Response of Heavy Planetary Ions at Mars to Reversals of the IMF

Author

Curry, Shannon, Dong, Chuanfei, Luhmann, Janet, Ma, Yingjuan, Bougher, Stephen, Modolo, Ronan, Leblanc, François, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley], and University of California-University of California

Subjects
Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

International audience; We present a kinetic study to quantify the response of Mars’ atmosphere to changes in the interplanetary magnetic field (IMF) configuration, specifically with respect to the escape rate of the atmosphere. Because Mars lacks a dipole magnetic field, the solar wind directly interacts with the upper neutral atmosphere to create ‘pick-up’ ions. We will present global maps of escaping O+ pick up ions during different solar cycle phases for multiple IMF conditions using a magnetohydrodynamic (MHD) and test particle simulation. This study also examines the role of the crustal fields for the different IMF configurations; the remanent crustal magnetic fields, especially in extreme conditions, influence the magnetic topology at Mars and subsequently drive changes in heavy ion atmospheric escape. The results indicate that the escape rate from Mars’ atmosphere can change over an order of magnitude due to the IMF, solar cycle, and crustal field orientation, directly impacting Mars’ climate and our understanding of the processes that influence atmospheric evolution. These results directly support MAVEN, the next Mars Scout, whose primary objective is to understand the evolution of Mars’ atmosphere.

Published
2014

176. Deep nightside photoelectron observations by MAVEN SWEA: Implications for Martian northern hemispheric magnetic topology and nightside ionosphere source

Author

Xu, Shaosui, primary, Mitchell, David, additional, Liemohn, Michael, additional, Dong, Chuanfei, additional, Bougher, Stephen, additional, Fillingim, Matthew, additional, Lillis, Robert, additional, McFadden, James, additional, Mazelle, Christian, additional, Connerney, Jack, additional, and Jakosky, Bruce, additional

Published
2016
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180. Implications of MAVEN Mars near‐wake measurements and models

Author

Luhmann, J. G., primary, Dong, Chuanfei, additional, Ma, Yingjuan, additional, Curry, S. M., additional, Mitchell, D., additional, Espley, J., additional, Connerney, J., additional, Halekas, J., additional, Brain, D. A., additional, Jakosky, B. M., additional, and Mazelle, C., additional

Published
2015
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182. Multifluid MHD study of the solar wind interaction with Mars' upper atmosphere during the 2015 March 8th ICME event

Author

Dong, Chuanfei, primary, Ma, Yingjuan, additional, Bougher, Stephen W., additional, Toth, Gabor, additional, Nagy, Andrew F., additional, Halekas, Jasper S., additional, Dong, Yaxue, additional, Curry, Shannon M., additional, Luhmann, Janet G., additional, Brain, David, additional, Connerney, Jack E. P., additional, Espley, Jared, additional, Mahaffy, Paul, additional, Benna, Mehdi, additional, McFadden, James P., additional, Mitchell, David L., additional, DiBraccio, Gina A., additional, Lillis, Robert J., additional, Jakosky, Bruce M., additional, and Grebowsky, Joseph M., additional

Published
2015
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198. PARKER SOLAR PROBE VENUS FLYBY CAMPAIGN: LATEST RESULTS.

Author

Curry, Shannon, Gruesbeck, Jacob, Luhmann, Janet, Rahmati, Ali, Goodrich, Katherine, Livi, Roberto, Whittlesey, Phyllis, Dong, Chuanfei, Yingjuan Ma, Malaspina, David, Pulupa, Marc, Bale, Stuart, Case, Anthony, Larson, Davin, Bonnell, John, MacDowall, Robert, and Stevens, Michael

Subjects
COMETS, ALBEDO, SMALL solar system bodies, SPACE sciences, SPACE environment, VENUS (Planet)
Published
2021

200. Mars: new insights and unresolved questions

Author

Changela, Hitesh G., Chatzitheodoridis, Elias, Antunes, Andre, Beaty, David, Bouw, Kristian, Bridges, John C., Capova, Klara Anna, Cockell, Charles S., Conley, Catharine A., Dadachova, Ekaterina, Dallas, Tiffany D., de Mey, Stefaan, Dong, Chuanfei, Ellery, Alex, Ferus, Martin, Foing, Bernard, Fu, Xiaohui, Fujita, Kazuhisa, Lin, Yangtin, Jheeta, Sohan, Hicks, Leon J., Hu, Sen, Kereszturi, Akos, Krassakis, Alexandros, Liu, Yang, Oberst, Juergen, Michalski, Joe, Ranjith, P. M., Rinaldi, Teresa, Rothery, David, Stavrakakis, Hector A., Selbmann, Laura, Sinha, Rishitosh K., Wang, Alian, Williford, Ken, Vaci, Zoltan, Vago, Jorge L., Waltemathe, Michael, Hallsworth, John E., Changela, Hitesh G., Chatzitheodoridis, Elias, Antunes, Andre, Beaty, David, Bouw, Kristian, Bridges, John C., Capova, Klara Anna, Cockell, Charles S., Conley, Catharine A., Dadachova, Ekaterina, Dallas, Tiffany D., de Mey, Stefaan, Dong, Chuanfei, Ellery, Alex, Ferus, Martin, Foing, Bernard, Fu, Xiaohui, Fujita, Kazuhisa, Lin, Yangtin, Jheeta, Sohan, Hicks, Leon J., Hu, Sen, Kereszturi, Akos, Krassakis, Alexandros, Liu, Yang, Oberst, Juergen, Michalski, Joe, Ranjith, P. M., Rinaldi, Teresa, Rothery, David, Stavrakakis, Hector A., Selbmann, Laura, Sinha, Rishitosh K., Wang, Alian, Williford, Ken, Vaci, Zoltan, Vago, Jorge L., Waltemathe, Michael, and Hallsworth, John E.

Abstract

Mars exploration motivates the search for extraterrestrial life, the development of space technologies, and the design of human missions and habitations. Here, we seek new insights and pose unresolved questions relating to the natural history of Mars, habitability, robotic and human exploration, planetary protection, and the impacts on human society. Key observations and findings include: – high escape rates of early Mars’ atmosphere, including loss of water, impact present-day habitability; – putative fossils on Mars will likely be ambiguous biomarkers for life; – microbial contamination resulting from human habitation is unavoidable; and – based on Mars’ current planetary protection category, robotic payload(s) should characterize the local martian environment for any life-forms prior to human habitation. Some of the outstanding questions are: – which interpretation of the hemispheric dichotomy of the planet is correct; – to what degree did deep-penetrating faults transport subsurface liquids to Mars’ surface; – in what abundance are carbonates formed by atmospheric processes; – what properties of martian meteorites could be used to constrain their source locations; – the origin(s) of organic macromolecules; – was/is Mars inhabited; – how can missions designed to uncover microbial activity in the subsurface eliminate potential false positives caused by microbial contaminants from Earth; – how can we ensure that humans and microbes form a stable and benign biosphere; and – should humans relate to putative extraterrestrial life from a biocentric viewpoint (preservation of all biology), or anthropocentric viewpoint of expanding habitation of space? Studies of Mars’ evolution can shed light on the habitability of extrasolar planets. In addition, Mars exploration can drive future policy developments and

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