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1. The CRISM investigation in Mars orbit: Overview, history, and delivered data products

Author

Seelos, Frank P., Seelos, Kimberly D., Murchie, Scott L., Novak, M. Alexandra Matiella, Hash, Christopher D., Morgan, M. Frank, Arvidson, Raymond E., Aiello, John, Bibring, Jean-Pierre, Bishop, Janice L., Boldt, John D., Boyd, Ariana R., Buczkowski, Debra L., Chen, Patrick Y., Clancy, R. Todd, Ehlmann, Bethany L., Frizzell, Katelyn, Hancock, Katie M., Hayes, John R., Heffernan, Kevin J., Humm, David C., Itoh, Yuki, Ju, Maggie, Kochte, Mark C., Malaret, Erick, McGovern, J. Andrew, McGuire, Patrick, Mehta, Nishant L., Moreland, Eleanor L., Mustard, John F., Nair, A. Hari, Núñez, Jorge I., O'Sullivan, Joseph A., Packer, Liam L., Poffenbarger, Ryan T., Poulet, Francois, Romeo, Giuseppe, Santo, Andrew G., Smith, Michael D., Stephens, David C., Toigo, Anthony D., Viviano, Christina E., and Wolff, Michael J.

Published
2024
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7. The CRISM investigation in Mars orbit: Overview, history, and delivered data products

Author

Seelos, Frank P., primary, Seelos, Kimberly D., additional, Murchie, Scott L., additional, Novak, M. Alexandra Matiella, additional, Hash, Christopher D., additional, Morgan, M. Frank, additional, Arvidson, Raymond E., additional, Aiello, John, additional, Bibring, Jean-Pierre, additional, Bishop, Janice L., additional, Boldt, John D., additional, Boyd, Ariana R., additional, Buczkowski, Debra L., additional, Chen, Patrick Y., additional, Clancy, R. Todd, additional, Ehlmann, Bethany L., additional, Frizzell, Katelyn, additional, Hancock, Katie M., additional, Hayes, John R., additional, Heffernan, Kevin J., additional, Humm, David C., additional, Itoh, Yuki, additional, Ju, Maggie, additional, Kochte, Mark C., additional, Malaret, Erick, additional, McGovern, J. Andrew, additional, McGuire, Patrick, additional, Mehta, Nishant L., additional, Moreland, Eleanor L., additional, Mustard, John F., additional, Nair, A. Hari, additional, Núñez, Jorge I., additional, O'Sullivan, Joseph A., additional, Packer, Liam L., additional, Poffenbarger, Ryan T., additional, Poulet, Francois, additional, Romeo, Giuseppe, additional, Santo, Andrew G., additional, Smith, Michael D., additional, Stephens, David C., additional, Toigo, Anthony D., additional, Viviano, Christina E., additional, and Wolff, Michael J., additional

Published
2023
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21. Vertical Profiles of Mars 1.27 Micrometer O2 Dayglow from MRO CRISM Limb Spectra: Seasonal/global Behaviors, Comparisons to LMDGCM Simulations, and a Global Definition for Mars Water Vapor Profiles

Author

Clancy, R. Todd, Smith, Michael D, Lefevre, Franck, McConnochie, Timothy H, Sandor, Brad J, Wolff, Michael J, Lee, Steven W, Murchie, Scott L, Toigo, Anthony D, Nair, Hari, and Navarro, Thomas

Subjects
Lunar And Planetary Science And Exploration
Abstract

Since July of 2009, The Compact Reconnaissance Imaging Spectral Mapper (CRISM) onboard the Mars Re- connaissance Orbiter (MRO) has periodically obtained pole-to-pole observations (i.e., full MRO orbits) of limb scanned visible/near IR spectra (lambda= 0.4 - 4.0 micrometers, delta lambda approx. 10 nm- Murchie et al., 2007). These CRISM limb observations support the first seasonally and spatially extensive set of Mars 1.27 micometers O2 (1 delta(sub g)) day-glow profile retrievals (approx. 1100) over greater than or equal to 8-80 km altitudes. Their comparison to Laboratoire de Meteorologie Dynamique (LMD) global climate model (GCM) simulated O2 (1 delta(sub g)) volume emission rate (VER) profiles, as a function of altitude, latitude, and season (solar longitude, L(sub s), supports several key conclusions regarding Mars atmospheric water vapor (which is derived from O2 (1 delta(sub g)) emission rates), Mars O3, and the collisional de-excitation of O2 (1 delta(sub g)) in the Mars CO2 atmosphere. Current (Navarro et al., 2014) LMDGCM simulations of Mars atmospheric water vapor fall 2-3 times below CRISM derived water vapor abundances at 20-40 km altitudes over low-to-mid latitudes in northern spring (L(sub s) = 30-60 deg), and northern mid-to-high latitudes over northern summer (L(sub s) = 60-140 deg). In contrast, LMDGCM simulated water vapor is 2-5 times greater than CRISM derived values at all latitudes and seasons above 40 km, within the aphelion cloud belt (ACB), and over high-southern to mid-southern latitudes in southern summer (L(sub s) = 190-340 deg) at 15-35 km altitudes. Overall, the solstitial summer-to-winter hemisphere gradients in water vapor are reversed between the LMDGCM modeled versus the CRISM derived water vapor abundances above 10-30 km altitudes. LMDGCM-CRISM differences in water vapor profiles correlate with LMDGCM-CRISM differences in cloud mixing profiles; and likely reflect limitations in simulating cloud microphysics and radiative forcing, both of which restrict meridional transport of water from summer- to-winter hemispheres on Mars (Clancy et al., 1996; Montmessin et al., 2004; Steele et al., 2014; Navarro et al., 2014) and depend on uncertain cloud microphysical properties (Navarro et al., 2014). The derived low-to-mid latitude changes in Mars water vapor vertical distributions should reduce current model- data disagreements in column O3 and H2O2 abundances over low-to-mid latitudes (e.g., within the ACB; Lefevre et al., 2008; Encrenaz et al., 2015; Clancy et al., 2016). Lastly, the global/seasonal average com- parison of CRISM and LMDGCM O2 (1 delta(sub g)) VER below 20 km altitudes indicates a factor of approx. 3 times lower value (0.25 x 10(exp -20) cu cm sec(exp -1)) for the CO2 collisional de-excitation rate coefficient of O2 (1 delta(sub g)) than derived recently by Guslyakova et al. (2016).

Published
2017
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23. Large Eddy Simulations of the Dusty Martian Convective Boundary Layer With MarsWRF

Author

Wu, Zhaopeng, primary, Richardson, Mark I., additional, Zhang, Xi, additional, Cui, Jun, additional, Heavens, Nicholas G., additional, Lee, Christopher, additional, Li, Tao, additional, Lian, Yuan, additional, Newman, Claire E., additional, Soto, Alejandro, additional, Temel, Orkun, additional, Toigo, Anthony D., additional, and Witek, Marcin, additional

Published
2021
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24. Thermal tides on Pluto

Author

Toigo, Anthony D., Gierasch, Peter J., Sicardy, Bruno, and Lellouch, Emmanuel

Subjects
Planets -- Atmosphere, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2010.01.027 Byline: Anthony D. Toigo (a), Peter J. Gierasch (b), Bruno Sicardy (c), Emmanuel Lellouch (c) Keywords: Pluto, Atmosphere; Tides, Atmospheric; Occultations; Pluto; Atmospheres, Structure Abstract: Stellar occultations have shown that vertical profiles of density fluctuations in the atmosphere of Pluto typically show wave-like structure with an amplitude of a few percent and vertical wavelengths of a few kilometers. Here we calculate the tidal response of Pluto's atmosphere to solar-induced sublimation 'breathing' from N.sub.2 frost patches. Solutions show global-scale wave-like density structure capable of explaining the observations. The atmospheric response is a combination of eastward and westward migrating tides, together with a zonally symmetric mode. Calculated vertical wavelengths and amplitudes are similar to observations. Author Affiliation: (a) Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853-6801, United States (b) Astronomy Department, Cornell University, Ithaca, NY 14853-6801, United States (c) LESIA, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France Article History: Received 31 July 2009; Revised 19 January 2010; Accepted 25 January 2010

Published
2010

25. Thermal Tides During the 2001 Martian Global-Scale Dust Storm

Author

Guzewich, Scott D, Wilson, R. John, McConnochie, Timothy H, Toigo, Anthony D, Bandfield, Donald J, and Smith, Michael D

Subjects
Lunar And Planetary Science And Exploration, Geosciences (General)
Abstract

The 2001 (Mars Year 25) global dust storm radically altered the dynamics of the Martian atmosphere. Using observations from the Thermal Emission Spectrometer onboard the Mars Global Surveyor spacecraft and Mars WRF general circulation model simulations, we examine the changes to thermal tides and planetary waves caused by the storm. We find that the extratropical diurnal migrating tide is dramatically enhanced during the storm, particularly in the southern hemisphere, reaching amplitudes of more than 20 K. The tropical diurnal migrating tide is weakened to almost undetectable levels. The diurnal Kelvin waves are also significantly weakened, particularly during the period of global expansion at Ls=200deg-210deg. In contrast, the westward propagating diurnal wavenumber 2 tide strengthens to 4-8 K at altitudes above 30km. The wavenumber 1 stationary wave reaches amplitudes of 10-12 K at 50deg-70degN, far larger than is typically seen during this time of year. The phase of this stationary wave and the enhancement of the diurnal wavenumber 2 tide appear to be responses to the high-altitude westward propagating equatorial wavenumber 1 structure in dust mixing ratio observed during the storm in previous works. This work provides a global picture of dust storm wave dynamics that reveals the coupling between the tropics and high-latitude wave responses. We conclude that the zonal distribution of thermotidal forcing from atmospheric aerosol concentration is as important to understanding the atmospheric wave response as the total global mean aerosol optical depth.

Published
2014
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27. Eolian controlled modification of the martian south polar layered deposits

Author

Koutnik, Michelle R., Byrne, Shane, Murray, Bruce C., Toigo, Anthony D., and Crawford, Zane A.

Subjects
Astrogeology -- Research, Polar regions -- Observations, Polar regions -- Natural history, Mars (Planet) -- Observations, Mars (Planet) -- Natural history, Astronomy, Earth sciences
Abstract

Data from the Mars Orbiter Laser Altimeter (MOLA) and Mars Orbiter Camera (MOC) aboard the Mars Global Surveyor (MGS) mission and the Thermal Emission Imaging System (THEMIS) aboard the Mars Odyssey mission have revealed unique surface features in a particular region of the South Polar Layered Deposits (SPLD). The dominant morphology is large-scale quasi-parallel grooves that extend for hundreds of kilometers with only tens of meters of vertical relief, that we have termed here the 'Wire Brush' terrain. The grooves are also transected by disjointed, yet roughly continuous, low-relief sinuous ridges that cross roughly perpendicular to the trend-direction of the large-scale grooves and show only tens of meters of relief. We interpret these ridges to be eroded remnants of folded layers. At the northern end of the large-scale grooves there are non-symmetric mounds. They are frequently preceded by a significant depression and/or trailing grooves that are parallel to the Wire Brush trend. We find that a two-stage process involving winds that intermittently remove a low-density crust exposing the underlying ice to ablation is the interpretation that best explains the multitude of features observed here. These features appear to be currently inactive indicating higher winds in previous epochs. Keywords: Mars, surface; Ices; Wind; Polar

Published
2005

28. Extensive MRO CRISM Observations of 1.27 micron O2 Airglow in Mars Polar Night and Their Comparison to MRO MCS Temperature Profiles and LMD GCM Simulations

Author

Clancy, R. Todd, Sandor, Brad J, Wolff, Michael J, Smith, Michael Doyle, Lefevre, Franck, Madeleine, Jean-Baptiste, Forget, Francois, Murchie, Scott L, Seelos, Frank P, Seelos, Kim D, Nair, Hari A, Toigo, Anthony D, Humm, David, Kass, David M, Kleinbahl, Armin, and Heavens, Nicholas

Subjects
Lunar And Planetary Science And Exploration
Abstract

The Martian polar night distribution of 1.27 micron (0-0) band emission from O2 singlet delta [O2(1Delta(sub g))] is determined from an extensive set of Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectral Mapping (CRISM) limb scans observed over a wide range of Mars seasons, high latitudes, local times, and longitudes between 2009 and 2011. This polar nightglow reflects meridional transport and winter polar descent of atomic oxygen produced from CO2 photodissociation. A distinct peak in 1.27 micron nightglow appears prominently over 70-90NS latitudes at 40-60 km altitudes, as retrieved for over 100 vertical profiles of O2(1Delta(sub g)) 1.27 micron volume emission rates (VER). We also present the first detection of much (x80+/-20) weaker 1.58 micron (0-1) band emission from Mars O2(1Delta(sub g)). Co-located polar night CRISM O2(1Delta(sub g)) and Mars Climate Sounder (MCS) (McCleese et al., 2008) temperature profiles are compared to the same profiles as simulated by the Laboratoire de Météorologie Dynamique (LMD) general circulation/photochemical model (e.g., Lefèvre et al., 2004). Both standard and interactive aerosol LMD simulations (Madeleine et al., 2011a) underproduce CRISM O2(1Delta(sub g)) total emission rates by 40%, due to inadequate transport of atomic oxygen to the winter polar emission regions. Incorporation of interactive cloud radiative forcing on the global circulation leads to distinct but insufficient improvements in modeled polar O2(1Delta(sub g)) and temperatures. The observed and modeled anti-correlations between temperatures and 1.27 mm band VER reflect the temperature dependence of the rate coefficient for O2(1Delta(sub g)) formation, as provided in Roble (1995).

Published
2012
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29. Martian weather correlation length scales

Author

Banfield, Don, Toigo, Anthony D., Ingersoll, Andrew P., and Paige, David A.

Subjects
Mars (Planet) -- Atmosphere, Planetary meteorology -- Research, Astronomy, Earth sciences
Published
1996

30. The Distinct and Surprisingly Diverse Populations and Properties of Mars Mesospheric Aerosols

Author

Clancy, R. T., Wolff, M. J., Smith, Michael D., Kleinboehl, Armin, Cantor, B. A., Seelos, Kim D., Toigo, Anthony D., Murchie, Scott L., Daerden, Frank, Montmessin, Franck, Lefèvre, Franck, Cardon, Catherine, Space Science Institute [Boulder] (SSI), NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Malin Space Science Systems (MSSS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Planetary meteorology, Mars, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract

International audience; Analysis of a 2009-2016 set of MRO CRISM limb observations and contemporaneous MCS and MARCI observations yields a new and uniquely comprehensive characterization of dust and ice aerosol distributions and physical characteristics in the Mars mesosphere (50-100 km). Key conclusions are: [1] very distinct aphelion (Ls=0-160º) and perihelion (Ls=160-360º) aerosol populations, in which low latitude CO2 clouds at 60-70 km altitudes dominate the aphelion mesosphere and H2O ice clouds at 50-75 km altitudes dominate the perihelion mesosphere; [2] mesospheric H2O clouds composed of small particle sizes (Reff=0.2 μm) and CO2 cloud particles exhibiting a very broad range of particle sizes (Reff=0.3-2.5 μm) with small particle sizes prominent at the latitude/altitude boundaries of mesospheric CO2 cloud formation; [3] infrequent mesospheric dust aerosols in these non-planet encircling dust storm years with small particle sizes (Reff=0.3-0.6 μm); [4] MCS temperature measurements indicating saturation conditions in the vicinity of mesospheric ice aerosols and enhanced solar heating in the presence of dust aerosols; [5] very narrow CO2 particle size distributions (Veff=0.01-0.03) indicative of iridescence and rapid, uniform cloud nucleation; [6] MCS-CRISM comparisons indicating comparable daytime (3pm) CO2 cloud particle sizes but also MCS nighttime (3am) measurements indicating pervasive low latitude mesospheric CO2 clouds at lower altitudes (55-65 km) and with larger particle sizes (Reff=4-6 μm); [7] MARCI imaging of mesospheric ice clouds displaying wave forms indicative of gravity-wave forcing; and [8] strong indications that cloud nucleation centers, whatever they may be, are not lacking in Mars' mesosphere.

Published
2018

31. The Martian planetary boundary layer

Author

Read, Peter L., Larsen, Soren E., Lewis, Stephen R., Määttänen, Anni, Petrosyan, Arakel, Renno, Nilton, Savijärvi, Hannu, Siili, Tero, Spiga, Aymeric, Toigo, Anthony D., Vazquez, Luis, Wind Energy Division [Roskilde], Risø National Laboratory for Sustainable Energy (Risø DTU), Technical University of Denmark [Lyngby] (DTU)-Technical University of Denmark [Lyngby] (DTU), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), PLANETO - 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), Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Finnish Meteorological Institute (FMI), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Robert M. Haberle, R. Todd Clancy, François Forget, Michael D. Smith, Richard W. Zurek (eds.), Danmarks Tekniske Universitet = Technical University of Denmark (DTU)-Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), and Cardon, Catherine

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

International audience

Published
2017

32. Vertical profiles of Mars 1.27 µm O 2 dayglow from MRO CRISM limb spectra: Seasonal/global behaviors, comparisons to LMDGCM simulations, and a global definition for Mars water vapor profiles

Author

Todd Clancy, R., primary, Smith, Michael D., additional, Lefèvre, Franck, additional, McConnochie, Timothy H., additional, Sandor, Brad J., additional, Wolff, Michael J., additional, Lee, Steven W., additional, Murchie, Scott L., additional, Toigo, Anthony D., additional, Nair, Hari, additional, and Navarro, Thomas, additional

Published
2017
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33. Correction to 'Extensive MRO CRISM observations of 1.27 µm O2 airglow in Mars polar night and their comparison to MRO MCS temperature profiles and LMD GCM simulations'

Author

Clancy, R. Todd, Sandor, Brad J., Wolff, Michael J., Smith, Michael D., Lefèvre, Franck, Madeleine, Jean-Baptiste, Forget, François, Murchie, Scott L., Seelos, Frank, Seelos, Kim D., Nair, Hari A., Toigo, Anthony D., Humm, David, Kass, David M., Kleinböhl, Armin, Heavens, Nicholas, Space Science Institute [Boulder] (SSI), NASA Goddard Space Flight Center (GSFC), PLANETO - 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), Institut Pierre-Simon-Laplace (IPSL), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Pierre et Marie Curie - Paris 6 (UPMC), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), École normale supérieure - Paris (ENS Paris), Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2013

34. Extensive MRO CRISM observations of 1.27 μm O2 airglow in Mars polar night and their comparison to MRO MCS temperature profiles and LMD GCM simulations

Author

Clancy, R. Todd, Sandor, Brad J., Wolff, Michael J., Smith, Michael D., Lefèvre, Franck, Madeleine, Jean-Baptiste, Forget, François, Murchie, Scott L., Seelos, Frank, Seelos, Kim D., Nair, Hari A., Toigo, Anthony D., Humm, David, Kass, David M., Kleinböhl, Armin, Heavens, Nicholas, Space Science Institute [Boulder] (SSI), NASA Goddard Space Flight Center (GSFC), PLANETO - 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), Institut Pierre-Simon-Laplace (IPSL), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Pierre et Marie Curie - Paris 6 (UPMC), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), École normale supérieure - Paris (ENS-PSL), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
Singlet delta, O2, Photochemistry, Atmosphere, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Polar
Abstract

International audience; The Martian polar night distribution of 1.27 μm (0-0) band emission from O2 singlet delta [O2(1Δg)] is determined from an extensive set of Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectral Mapping (CRISM) limb scans observed over a wide range of Mars seasons, high latitudes, local times, and longitudes between 2009 and 2011. This polar nightglow reflects meridional transport and winter polar descent of atomic oxygen produced from CO2 photodissociation. A distinct peak in 1.27 μm nightglow appears prominently over 70-90NS latitudes at 40-60 km altitudes, as retrieved for over 100 vertical profiles of O2(1Δg) 1.27 μm volume emission rates (VER). We also present the first detection of much (x80±20) weaker 1.58 μm (0-1) band emission from Mars O2(1Δg). Co-located polar night CRISM O2(1Δg) and Mars Climate Sounder (MCS, McCleese et al, 2007) temperature profiles are compared to the same profiles as simulated by the Laboratoire de Meteorologie Dynamique (LMD) general circulation/photochemical model (e.g., Lefevre et al, 2004). Both standard and interactive aerosol LMD simulations (Madeleine et al, 2011) underproduce CRISM O2(1Δg) total emission rates by 40%, due to inadequate transport of atomic oxygen to the winter polar emission regions. Incorporation of interactive cloud radiative forcing on the global circulation leads to distinct but insufficient improvements in modeled polar O2(1Δg) and temperatures. The observed and modeled anti-correlations between temperatures and 1.27 μm band VER reflect the temperature dependence of the rate coefficient for O2(1Δg) formation, as provided in Roble (1995).

Published
2012

35. Recurring slope lineae in equatorial regions of Mars

Author

McEwen, Alfred S., primary, Dundas, Colin M., additional, Mattson, Sarah S., additional, Toigo, Anthony D., additional, Ojha, Lujendra, additional, Wray, James J., additional, Chojnacki, Matthew, additional, Byrne, Shane, additional, Murchie, Scott L., additional, and Thomas, Nicolas, additional

Published
2013
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39. Extensive MRO CRISM observations of 1.27 μm O2 airglow in Mars polar night and their comparison to MRO MCS temperature profiles and LMD GCM simulations

Author

Clancy, R. Todd, primary, Sandor, Brad J., additional, Wolff, Michael J., additional, Smith, Michael D., additional, Lefèvre, Franck, additional, Madeleine, Jean‐Baptiste, additional, Forget, Francois, additional, Murchie, Scott L., additional, Seelos, Frank P., additional, Seelos, Kim D., additional, Nair, Hari A., additional, Toigo, Anthony D., additional, Humm, David, additional, Kass, David M., additional, Kleinböhl, Armin, additional, and Heavens, Nicholas, additional

Published
2012
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49. Recurring slope lineae in equatorial regions of Mars.

Author

McEwen, Alfred S., Dundas, Colin M., Mattson, Sarah S., Toigo, Anthony D., Ojha, Lujendra, Wray, James J., Chojnacki, Matthew, Byrne, Shane, Murchie, Scott L., and Thomas, Nicolas

Subjects
SLOPES (Physical geography), OBSERVATIONS of Mars, MARTIAN exploration, LIQUID surfaces
Abstract

The presence of liquid water is a requirement of habitability on a planet. Possible indicators of liquid surface water on Mars include intermittent flow-like features observed on sloping terrains. These recurring slope lineae are narrow, dark markings on steep slopes that appear and incrementally lengthen during warm seasons on low-albedo surfaces. The lineae fade in cooler seasons and recur over multiple Mars years. Recurring slope lineae were initially reported to appear and lengthen at mid-latitudes in the late southern spring and summer and are more common on equator-facing slopes where and when the peak surface temperatures are higher. Here we report extensive activity of recurring slope lineae in equatorial regions of Mars, particularly in the deep canyons of Valles Marineris, from analysis of data acquired by the Mars Reconnaissance Orbiter. We observe the lineae to be most active in seasons when the slopes often face the sun. Expected peak temperatures suggest that activity may not depend solely on temperature. Although the origin of the recurring slope lineae remains an open question, our observations are consistent with intermittent flow of briny water. Such an origin suggests surprisingly abundant liquid water in some near-surface equatorial regions of Mars. [ABSTRACT FROM AUTHOR]

Published
2014
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