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1. Measuring Mars Atmospheric Winds From Orbit

Author

Baker, Scott Guzewich J. B. Abshire. M. M., Battalio, J. M., Bertrand, T., Brown, A. J., Colaprete, A., Cook, A. M., Cremons, D. R., Crismani, M. M., Dave, A. I., Day, M., Desjean, M. -C., Elrod, M., Fenton, L. K., Fisher, J., Gordley, L. L., Hayne, P. O., Heavens, N. G., Hollingsworth, J. L., Jha, D., Jha, V., Kahre, M. A., Khayat, A. SJ., Kling, A. M., Lewis, S. R., Marshall, B. T., Martínez, G., Montabone, L., Mischna, M. A., Newman, C. E., Pankine, A., Riris, H., Shirley, J., Smith, M. D., Spiga, A., Sun, X., Tamppari, L. K., Young, R. M. B., Viúdez-Moreiras, D., Villaneuva, G. L., Wolff, M. J., and Wilson, R. J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Wind is the process that connects Mars' climate system. Measurements of Mars atmospheric winds from orbit would dramatically advance our understanding of Mars and help prepare for human exploration of the Red Planet. Multiple instrument candidates are in development and will be ready for flight in the next decade. We urge the Decadal Survey to make these measurements a priority for 2023-2032., Comment: A White Paper submitted to the Planetary Science and Astrobiology Decadal Survey 2023-2032

Published
2020

2. Martian water loss to space enhanced by regional dust storms

Author

Chaffin, M. S., Kass, D. M., Aoki, S., Fedorova, A. A., Deighan, J., Connour, K., Heavens, N. G., Kleinböhl, A., Jain, S. K., Chaufray, J.-Y., Mayyasi, M., Clarke, J. T., Stewart, A. I. F., Evans, J. S., Stevens, M. H., McClintock, W. E., Crismani, M. M. J., Holsclaw, G. M., Lefevre, F., Lo, D. Y., Montmessin, F., Schneider, N. M., Jakosky, B., Villanueva, G., Liuzzi, G., Daerden, F., Thomas, I. R., Lopez-Moreno, J.-J., Patel, M. R., Bellucci, G., Ristic, B., Erwin, J. T., Vandaele, A. C., Trokhimovskiy, A., and Korablev, O. I.

Published
2021
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3. The Role and Lifetime of Dissociative Heterogeneous Processes in Improving Simulated Ozone on Mars.

Author

Brown, M. A. J., Patel, M. R., Lewis, S. R., Holmes, J. A., Lefèvre, F., Mason, J. P., and Crismani, M.

Subjects
CLIMATE change models, GASES, TRACE gases, MARTIAN atmosphere, RADICALS (Chemistry)
Abstract

Ozone simulated in Mars Global Climate Models (MGCMs) is used to assess the underlying chemistry occurring in the atmosphere. Currently, ozone total column abundance (TCA) is under‐predicted in MGCMs by up to 120%, implying missing or inaccurate chemistry in models. Heterogeneous reactions of hydroxyl radicals (HOX) have been offered as an explanation for some of this bias, because they cause ozone to increase at locations where it's currently under‐predicted. We use four simulations to compare modeled ozone TCA with observations from the UVIS spectrometer aboard the ExoMars Trace Gas Orbiter to improve the representation of heterogeneous processes and their impact on ozone. We use a gas‐phase only run, a dissociative scheme, an adsorbed HOX retention scheme, and a hybrid scheme that combines the dissociative mechanism with the retention of HOX on water ice. We find retention of HOX is dependent on water ice sublimation, and ozone abundance increases when water ice persists for longer periods (1–20 sols). Over time, the loss of HOX causes a depletion in H2O2 concentration (HOX reservoir), and thus allows ozone concentration to increase. When adsorbed HOX are desorbed and dissociate into other by‐products, HOX are not immediately available to destroy ozone. This results in larger ozone concentrations than if desorbed HOX are released directly back into their gaseous states. When using the hybrid scheme, ozone TCA is increased up to 50% where the ozone deficit is greatest, demonstrating the best agreement with observations, and implying that HOX radicals are both retained when adsorbed and dissociate. Plain Language Summary: Ozone is a trace gas in the martian atmosphere, sensitive to chemical and light‐induced reactions. This makes it ideal for assessing the underlying reactions for chemical species called hydroxyl radicals, which destroy ozone and would otherwise be too reactive and shortlived to be measured directly. There has been an under‐prediction of ozone in global climate models which implies missing or inaccurate reactions. Heterogeneous reactions (a reaction which includes two or more phases) have been suggested to fill the deficit in modeled ozone. This involves hydroxyl radicals adsorbing onto water ice, which causes ozone to increase. We look at different simulations to understand hydroxyl radical chemistry on the surface of water ice by comparing to observations from the ExoMars Trace Gas Orbiter. We run four climate model simulations to test different theories as to what is occurring at the surface. There are two theories (a) reactions happen at the surface which alter hydroxyl radicals into other chemicals, and (b) hydroxyl radicals stay adsorbed onto water ice for as long as the ice persists. When we combine these theories, we have a more accurate prediction of ozone, which we can then use to infer what happens at the surface. Key Points: Heterogeneous reactions can have a major impact on martian ozone abundance at locations where water ice clouds persist for several solsLifetime of adsorbed hydroxyl radicals depends on water ice sublimation and longer lifetimes result in a greater abundance of ozoneA combination of longer lifetimes and dissociation of adsorbed HOX suppresses gaseous HOX and improves simulated ozone total column abundance [ABSTRACT FROM AUTHOR]

Published
2024
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4. Discovery of a proton aurora at Mars

Author

Deighan, J., Jain, S. K., Chaffin, M. S., Fang, X., Halekas, J. S., Clarke, J. T., Schneider, N. M., Stewart, A. I. F., Chaufray, J.-Y., Evans, J. S., Stevens, M. H., Mayyasi, M., Stiepen, A., Crismani, M., McClintock, W. E., Holsclaw, G. M., Lo, D. Y., Montmessin, F., Lefèvre, F., and Jakosky, B. M.

Published
2018
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6. Early MAVEN Deep Dip campaign reveals thermosphere and ionosphere variability

Author

Bougher, S., Jakosky, B., Halekas, J., Grebowsky, J., Luhmann, J., Mahaffy, P., Connerney, J., Eparvier, F., Ergun, R., Larson, D., McFadden, J., Mitchell, D., Schneider, N., Zurek, R., Mazelle, C., Andersson, L., Andrews, D., Baird, D., Baker, D. N., Bell, J. M., Benna, M., Brain, D., Chaffin, M., Chamberlin, P., Chaufray, J.-Y., Clarke, J., Collinson, G., Combi, M., Crary, F., Cravens, T., Crismani, M., Curry, S., Curtis, D., Deighan, J., Delory, G., Dewey, R., DiBraccio, G., Dong, C., Dong, Y., Dunn, P., Elrod, M., England, S., Eriksson, A., Espley, J., Evans, S., Fang, X., Fillingim, M., Fortier, K., Fowler, C. M., Fox, J., Gröller, H., Guzewich, S., Hara, T., Harada, Y., Holsclaw, G., Jain, S. K., Jolitz, R., Leblanc, F., Lee, C. O., Lee, Y., Lefevre, F., Lillis, R., Livi, R., Lo, D., Ma, Y., Mayyasi, M., McClintock, W., McEnulty, T., Modolo, R., Montmessin, F., Morooka, M., Nagy, A., Olsen, K., Peterson, W., Rahmati, A., Ruhunusiri, S., Russell, C. T., Sakai, S., Sauvaud, J.-A., Seki, K., Steckiewicz, M., Stevens, M., Stewart, A. I. F., Stiepen, A., Stone, S., Tenishev, V., Thiemann, E., Tolson, R., Toublanc, D., Vogt, M., Weber, T., Withers, P., Woods, T., and Yelle, R.

Published
2015

7. Discovery of diffuse aurora on Mars

Author

Schneider, N. M., Deighan, J. I., Jain, S. K., Stiepen, A., Stewart, A. I. F., Larson, D., Mitchell, D. L., Mazelle, C., Lee, C. O., Lillis, R. J., Evans, J. S., Brain, D., Stevens, M. H., McClintock, W. E., Chaffin, M. S., Crismani, M., Holsclaw, G. M., Lefevre, F., Lo, D. Y., Clarke, J. T., Montmessin, F., and Jakosky, B. M.

Published
2015

8. MAVEN observations of the response of Mars to an interplanetary coronal mass ejection

Author

Jakosky, B. M., Grebowsky, J. M., Luhmann, J. G., Connerney, J., Eparvier, F., Ergun, R., Halekas, J., Larson, D., Mahaffy, P., McFadden, J., Mitchell, D. F., Schneider, N., Zurek, R., Bougher, S., Brain, D., Ma, Y. J., Mazelle, C., Andersson, L., Andrews, D., Baird, D., Baker, D., Bell, J. M., Benna, M., Chaffin, M., Chamberlin, P., Chaufray, Y.-Y., Clarke, J., Collinson, G., Combi, M., Crary, F., Cravens, T., Crismani, M., Curry, S., Curtis, D., Deighan, J., Delory, G., Dewey, R., DiBraccio, G., Dong, C., Dong, Y., Dunn, P., Elrod, M., England, S., Eriksson, A., Espley, J., Evans, S., Fang, X., Fillingim, M., Fortier, K., Fowler, C. M., Fox, J., Gröller, H., Guzewich, S., Hara, T., Harada, Y., Holsclaw, G., Jain, S. K., Jolitz, R., Leblanc, F., Lee, C. O., Lee, Y., Lefevre, F., Lillis, R., Livi, R., Lo, D., Mayyasi, M., McClintock, W., McEnulty, T., Modolo, R., Montmessin, F., Morooka, M., Nagy, A., Olsen, K., Peterson, W., Rahmati, A., Ruhunusiri, S., Russell, C. T., Sakai, S., Sauvaud, J.-A., Seki, K., Steckiewicz, M., Stevens, M., Stewart, A. I. F., Stiepen, A., Stone, S., Tenishev, V., Thiemann, E., Tolson, R., Toublanc, D., Vogt, M., Weber, T., Withers, P., Woods, T., and Yelle, R.

Published
2015

10. Explaining NOMAD D/H Observations by Cloud‐Induced Fractionation of Water Vapor on Mars

Author

Daerden, F., Neary, L., Villanueva, G., Liuzzi, G., Aoki, S., Clancy, R. T., Whiteway, J. A., Sandor, B. J., Smith, M. D., Wolff, M. J., Pankine, A., Khayat, A., Novak, R., Cantor, B., Crismani, M., Mumma, M. J., Viscardy, S., Erwin, J., Depiesse, C., Mahieux, A., Piccialli, A., Robert, S., Trompet, L., Willame, Y., Neefs, E., Thomas, I. R., Ristic, B., and Vandaele, A. C.

Subjects
Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous)
Published
2022

11. Martian Meteoric Mg+: Atmospheric Distribution and Variability From MAVEN/IUVS.

Author

Crismani, M. M. J., Tyo, R. M., Schneider, N. M., Plane, J. M. C., Feng, W., Carrillo‐Sánchez, J. D., Villanueva, G. L., Jain, S., Deighan, J., and Curry, S.

Subjects
INTERPLANETARY dust, ATMOSPHERIC boundary layer, MARTIAN atmosphere, ATMOSPHERIC chemistry, ATMOSPHERIC tides, ATMOSPHERIC deposition, ATMOSPHERE
Abstract

Since the discovery of atmospheric Mg+ on Mars in 2015 by the Mars Atmosphere and Volatile Evolution mission, there have been almost continuous observations of this meteoric ion layer in a variety of seasons, local times, and latitudes. Here, we present the most comprehensive set of observations of the persistent metal ion layer at Mars, constructing the first grand composite maps from pooled medians of subsamples of a metallic ion species. These maps demonstrate that Mg+ appears in almost all conditions when illuminated, with peak density values varying between 100 and 500 cm−3, dependent on season and local time. There exists significant latitudinal variation within a given season, indicating that Mg+ is not simply an inert tracer, but may instead be influenced by the meteoric input distribution and/or atmospheric dynamics and chemistry. Geographic maps of Mg+ density as a function of latitude and longitude indicate the influence of atmospheric tides, and there is no apparent correlation with remnant crustal magnetic fields. This work also presents counter‐intuitive results, such as a reduction of Mg+ ions in the northern hemisphere during Northern Winter in an apparent correlation with dust aerosols. Plain Language Summary: Metallic atoms in a planet's atmosphere are present when interplanetary dust particles burn up, releasing atomic species not typically found in the lower atmosphere. The discovery of a high altitude metallic layer on Mars in 2015 has led to continued monitoring in a variety of seasons across the entire planet. These results demonstrate that this magnesium ion (Mg+) layer appears throughout the year, with variations in peak abundances and layer heights, due to interactions with the background atmosphere. These variations track the dynamics of the middle atmosphere, providing insight into global climate patterns and may inform our understanding of seasonal deposition of interplanetary dust particles and their sources. This first‐order analysis supports future modeling efforts and provides model challenges to be understood, both of which can be explored in detail with time varying full planet climate modeling. Key Points: Eight Earth years of Mars Atmosphere and Volatile Evolution/Imaging Ultraviolet Spectrograph observations show that Mars' persistent meteoric metal ion layer is more dynamic than initially assumedMg+ layer peak altitude, abundance, and top and bottom side slopes vary significantly over the observed time periodThe relative absence of northern hemispheric Mg+ during southern summer is surprising and may be related to lower atmospheric dust loading [ABSTRACT FROM AUTHOR]

Published
2023
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12. A Global and Seasonal Perspective of Martian Water Vapor From ExoMars/NOMAD

Author

Crismani, M. M. J., primary, Villanueva, G. L., additional, Liuzzi, G., additional, Smith, M. D., additional, Knutsen, E. W., additional, Daerden, F., additional, Neary, L., additional, Mumma, M. J., additional, Aoki, S., additional, Trompet, L., additional, Thomas, I. R., additional, Ristic, B., additional, Bellucci, G., additional, Piccialli, A., additional, Robert, S., additional, Mahieux, A., additional, Lopez Moreno, J.‐J., additional, Sindoni, G., additional, Giuranna, M., additional, Patel, M. R., additional, and Vandaele, A. C., additional

Published
2021
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13. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

Author

Aoki, S., primary, Daerden, F., additional, Viscardy, S., additional, Thomas, I. R., additional, Erwin, J. T., additional, Robert, S., additional, Trompet, L., additional, Neary, L., additional, Villanueva, G. L., additional, Liuzzi, G., additional, Crismani, M. M. J., additional, Clancy, R. T., additional, Whiteway, J., additional, Schmidt, F., additional, Lopez‐Valverde, M. A., additional, Ristic, B., additional, Patel, M. R., additional, Bellucci, G., additional, Lopez‐Moreno, J.‐J., additional, Olsen, K. S., additional, Lefèvre, F., additional, Montmessin, F., additional, Trokhimovskiy, A., additional, Fedorova, A. A., additional, Korablev, O., additional, and Vandaele, A. C., additional

Published
2021
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14. Water heavily fractionated as it ascends on Mars as revealed by ExoMars/NOMAD

Author

Belgian Science Policy Office, European Space Agency, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, M. M. J., Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Smith, M.D., Mumma, M.J., Knutsen, E. W., Neary, L., Viscardy, S., Thomas, Ian R., López-Valverde, M. A., Ristic, Bojan, Patel, Manish R., Holmes, J. A., Bellucci, Giancarlo, López-Moreno, José Juan, Belgian Science Policy Office, European Space Agency, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, M. M. J., Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Smith, M.D., Mumma, M.J., Knutsen, E. W., Neary, L., Viscardy, S., Thomas, Ian R., López-Valverde, M. A., Ristic, Bojan, Patel, Manish R., Holmes, J. A., Bellucci, Giancarlo, and López-Moreno, José Juan

Abstract

Isotopic ratios and, in particular, the water D/H ratio are powerful tracers of the evolution and transport of water on Mars. From measurements performed with ExoMars/NOMAD, we observe marked and rapid variability of the D/H along altitude on Mars and across the whole planet. The observations (from April 2018 to April 2019) sample a broad range of events on Mars, including a global dust storm, the evolution of water released from the southern polar cap during southern summer, the equinox phases, and a short but intense regional dust storm. In three instances, we observe water at very high altitudes (>80 km), the prime region where water is photodissociated and starts its escape to space. Rayleigh distillation appears the be the driving force affecting the D/H in many cases, yet in some instances, the exchange of water reservoirs with distinctive D/H could be responsible. © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science.

Published
2021

15. A Global and Seasonal Perspective of Martian Water Vapor From ExoMars/NOMAD

Author

National Aeronautics and Space Administration (US), Belgian Science Policy Office, European Space Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), UK Space Agency, Agenzia Spaziale Italiana, National Fund for Scientific Research (Belgium), Crismani, M. M. J., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Knutsen, E. W., Daerden, Frank, Neary, L., Mumma, M.J., Aoki, Shohei, Trompet, L., Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Piccialli, A., Robert, S., Mahieux, A., López-Moreno, José Juan, Sindoni, G., Giuranna, M., Patel, Manish R., Vandaele, Ann Carine, National Aeronautics and Space Administration (US), Belgian Science Policy Office, European Space Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), UK Space Agency, Agenzia Spaziale Italiana, National Fund for Scientific Research (Belgium), Crismani, M. M. J., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Knutsen, E. W., Daerden, Frank, Neary, L., Mumma, M.J., Aoki, Shohei, Trompet, L., Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Piccialli, A., Robert, S., Mahieux, A., López-Moreno, José Juan, Sindoni, G., Giuranna, M., Patel, Manish R., and Vandaele, Ann Carine

Abstract

Slightly less than a Martian Year of nominal science (March 2018–January 2020) with the ExoMars Trace Gas Orbiter has furthered the ongoing investigation of dayside water vapor column abundance. These dayside observations span latitudes between 75°S and 75°N, and all longitudes, which can provide global snapshots of the total water column abundances. In addition to tracking the seasonal transport of water vapor between poles, geographic enhancements are noted, particularly in the southern hemisphere, both in Hellas Basin, and in other regions not obviously correlated to topography. We report consistent water vapor climatology with previous spacecraft observations, however, note a difference in total water vapor content is noted. Finally, we are unable to find evidence for substantial diurnal variation in the total dayside water vapor column. © 2021. American Geophysical Union. All Rights Reserved.

Published
2021

16. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

Author

Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, European Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Belgian Science Policy Office, National Aeronautics and Space Administration (US), UK Space Agency, Aoki, Shohei, Daerden, Frank, Viscardy, S., Thomas, Ian R., Erwin, Justin T., Robert, S., Trompet, L., Neary, L., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, M. M. J., Clancy, R. Todd, Whiteway, J., Schmidt, F., López-Valverde, M. A., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Olsen, K. S., Lefèvre, F., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A. A., Korablev, O., Vandaele, Ann Carine, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, European Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Belgian Science Policy Office, National Aeronautics and Space Administration (US), UK Space Agency, Aoki, Shohei, Daerden, Frank, Viscardy, S., Thomas, Ian R., Erwin, Justin T., Robert, S., Trompet, L., Neary, L., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, M. M. J., Clancy, R. Todd, Whiteway, J., Schmidt, F., López-Valverde, M. A., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Olsen, K. S., Lefèvre, F., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A. A., Korablev, O., and Vandaele, Ann Carine

Abstract

Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. The reported detection made in Martian Year 34 was transient, present several months after the global dust storm during the southern summer season. Here, we present the full data set of vertically resolved HCl detections obtained by the NOMAD instrument, which covers also Martian year 35. We show that the particular increase of HCl abundances in the southern summer season is annually repeated, and that the formation of HCl is independent from a global dust storm event. We also find that the vertical distribution of HCl is strikingly similar to that of water vapor, which suggests that the uptake by water ice clouds plays an important role. The observed rapid decrease of HCl abundances at the end of the southern summer would require a strong sink independent of photochemical loss. © 2021. American Geophysical Union.

Published
2021

17. Measuring Mars Atmospheric Winds from Orbit

Author

Guzewich, Scott, primary, Abshire, J. B., additional, Baker, M. M., additional, Battalio, J. M., additional, Bertrand, T., additional, Brown, A. J., additional, Colaprete, A., additional, Cook, A. M., additional, Cremons, D. R., additional, Crismani, M. M., additional, Dave, A.I., additional, Day, M., additional, Desjean, M.-C., additional, Elrod, M., additional, Fenton, L. K., additional, Fisher, J., additional, Gordley, L. L., additional, Hayne, P. O., additional, Heavens, N. G., additional, Hollingsworth, J. L., additional, Jha, D., additional, Jha, V., additional, Kahre, M. A., additional, Khayat, A. SJ., additional, Kling, A. M., additional, Lewis, S. R., additional, Marshall, B. T., additional, Martínez, G., additional, Montabone, L., additional, Mischna, M. A., additional, Newman, C. E., additional, Pankine, A., additional, Riris, H., additional, Shirley, J., additional, Smith, M. D., additional, Spiga, A., additional, Sun, X., additional, Tamppari, L. K., additional, Young, R. M. B., additional, Viúdez-Moreiras, D., additional, Villaneuva, G. L., additional, Wolff, M. J., additional, and Wilson, R. J., additional

Published
2021
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18. Solar-System-Wide Significance of Mars Polar Science

Author

Smith, Isaac, primary, Calvin, W. M., additional, Smith, D. E., additional, Hansen, C., additional, Diniega, S., additional, McEwen, A., additional, Thomas, N., additional, Banfield, D., additional, Titus, T. N., additional, Becerra, P., additional, Kahre, M., additional, Forget, F., additional, Hecht, M., additional, Byrne, S., additional, Hvidberg, C. S., additional, Hayne, P. O., additional, III, J. W. Head,, additional, Mellon, M., additional, Horgan, B., additional, Mustard, J., additional, Holt, J. W., additional, Howard, A., additional, McCleese, D., additional, Stoker, C., additional, James, P., additional, Putzig, N. E., additional, Whitten, J., additional, Buhler, P., additional, Spiga, A., additional, Crismani, M., additional, Aye, K. M., additional, Portyankina, A., additional, Orosei, R., additional, Bramson, A., additional, Hanley, J., additional, Sori, M., additional, Aharonson, O., additional, Clifford, S., additional, Sizemore, H., additional, Morgan, G., additional, Hartmann, B., additional, Schorghofer, N., additional, Clark, R., additional, Berman, D., additional, Crown, D., additional, Chuang, F., additional, Siegler, M., additional, Dobrea, E. N., additional, Lynch, K., additional, Obbard, R. W., additional, Elmaary, M. R., additional, Fisher, D., additional, Kleinboehl, A., additional, Balme, M., additional, Schmitt, B., additional, Daly, M., additional, Ewing, R. C., additional, Herkenhoff, K. E., additional, Fenton, L., additional, Guzewich, S. D., additional, Koutnik, M., additional, Levy, J., additional, Massey, R., additional, Łosiak, A., additional, Eke, V., additional, Goldsby, D., additional, Cross, A., additional, Hager, T., additional, Piqueux, S., additional, Kereszturi, A., additional, Seelos, K., additional, Wood, S., additional, Hauber, E., additional, Amos, C., additional, Russell, P., additional, Jaumann, R., additional, Michael, G., additional, Conway, S., additional, Khayat, A., additional, Lewis, S., additional, Luizzi, G., additional, Martinez, G., additional, Mesick, K., additional, Montabone, L., additional, Johnsson, A., additional, Pankine, A., additional, Phillips-Lander, C., additional, Read, P., additional, Edgar, L., additional, Zacny, K., additional, McAdam, A., additional, Rutledge, A., additional, Bertrand, T., additional, Widmer, J., additional, Stillman, D., additional, Soto, A., additional, Yoldi, Z., additional, Young, R., additional, Svensson, A., additional, Sam, L., additional, Landis, M., additional, Bhardwaj, A., additional, Chojnacki, M., additional, Kite, E., additional, Thomas, P., additional, Plaut, J., additional, Bapst, J., additional, Milkovich, S., additional, Whiteway, J., additional, Moores, J., additional, Rezza, C., additional, Karimova, R., additional, Mishev, I., additional, Brenen, A. Van, additional, Acharya, P., additional, Chesal, J., additional, Pascuzzo, A., additional, Vos, E., additional, Osinski, G., additional, Andres, C., additional, Neisch, C., additional, Hibbard, S., additional, Sinha, P., additional, Knightly, J. P., additional, Cartwright, S., additional, Kounaves, S., additional, Orgel, C., additional, Skidmore, M., additional, MacGregor, J., additional, Staehle, R., additional, Rabassa, J., additional, Gallagher, C., additional, Coronato, A., additional, Galofre, A. G., additional, Wilson, J., additional, McKeown, L., additional, Oliveira, N., additional, Fawdon, P., additional, Gayathri, U., additional, Stuurman, C., additional, Herny, C., additional, Butcher, F., additional, Bernardini, F., additional, Perry, M., additional, Hu, R., additional, Mukherjee, S., additional, Chevrier, V., additional, Banks, M. E., additional, Meng, T., additional, Johnson, P. A., additional, Tober, B., additional, Johnson, J. C., additional, Ulamsec, S., additional, Echaurren, J. C., additional, Khuller, A., additional, Dinwiddie, C., additional, Adeli, S., additional, Henderson, B. L., additional, Lozano, L. R., additional, Lalich, D., additional, Rivera-Valentín, E., additional, Nerozzi, S., additional, Petersen, E., additional, Foss, F., additional, Lorenz, R., additional, Eigenbrode, J., additional, Day, M., additional, Brown, A., additional, Pajola, M., additional, Karatekin, Ö., additional, Lucchetti, A., additional, Cesar, C., additional, Newman, C., additional, Cave, T. G., additional, Tamppari, L., additional, Mischna, M., additional, Patel, M., additional, Streeter, P., additional, Stern, J. C., additional, and Dundas, C. M., additional

Published
2021
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19. The Scientific Need for a Dedicated Interplanetary Dust Instrument at Mars

Author

Fries, Marc, primary, Ashley, J., additional, Beegle, L., additional, Bhartia, R., additional, Bland, P., additional, Burton, A., additional, Butterworth, A. L., additional, Cooke, W., additional, Conrad, P., additional, Christou, A., additional, Crismani, M., additional, Engrand, C., additional, Dartois, E., additional, Duprat, J., additional, Flynn, G., additional, Fisher, K., additional, Gainsforth, Z., additional, Genge, M., additional, Graham, L., additional, Horanyi, M., additional, Janches, D., additional, Kate, I. L. ten, additional, New, J. S., additional, Plane, J., additional, Rojas, J., additional, Sephton, M., additional, Steele, A., additional, Sykes, M., additional, Welzenbach, L., additional, and Zolensky, M., additional

Published
2021
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20. Explanation for the Increase in High‐Altitude Water on Mars Observed by NOMAD During the 2018 Global Dust Storm

Author

Neary, L., primary, Daerden, F., additional, Aoki, S., additional, Whiteway, J., additional, Clancy, R. T., additional, Smith, M., additional, Viscardy, S., additional, Erwin, J.T., additional, Thomas, I. R., additional, Villanueva, G., additional, Liuzzi, G., additional, Crismani, M., additional, Wolff, M., additional, Lewis, S. R., additional, Holmes, J. A., additional, Patel, M. R., additional, Giuranna, M., additional, Depiesse, C., additional, Piccialli, A., additional, Robert, S., additional, Trompet, L., additional, Willame, Y., additional, Ristic, B., additional, and Vandaele, A. C., additional

Published
2020
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21. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Smith, M.D., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, S., Gomez, A., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Perez-grande, I., Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), and Canadian Space Agency

Subjects
010504 meteorology & atmospheric sciences, Storm, Atmosphere of Mars, Mars Exploration Program, Atmospheric sciences, 01 natural sciences, Trace gas, Atmosphere, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Dust storm, Earth and Planetary Sciences (miscellaneous), Environmental science, Hadley cell, Water vapor, 0105 earth and related environmental sciences
Abstract

It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved., S. A. is >Charge de Recherches> of the F.R.S.-FNRS. ExoMars is a space mission of the European Space Agency and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASBBIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office, with the financial and contractual coordination by the European Space Agency Prodex Office (PEA 4000103401 and 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, and ST/S00145X/1 and Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and Belgian Science Policy Office BrainBe SCOOP Project. U.S. investigators were supported by the National Aeronautics and Space Administration. Canadian investigators were supported by the Canadian Space Agency. The results retrieved from the NOMAD measurements used in this article are available on the BIRA-IASB data repository: http://repository.aeronomie.be/?doi= 10.18758/71021054 (Aoki et al., 2019).

Published
2019

22. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, Gomez, A., Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, and Gomez, A.

Abstract

It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved.

Published
2019

23. Meteoric Metal Chemistry in the Martian Atmosphere

Author

Plane, J. M. C., Carrillo‐Sanchez, J. D., Mangan, T. P., Crismani, M. M. J., Schneider, N. M., Määttänen, A., School of Chemistry [Leeds], University of Leeds, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], 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), European Research Council, National planetology program PNP, CNES, IPSL, and European Project: 291332,EC:FP7:ERC,ERC-2011-ADG_20110209,CODITA(2012)

Subjects
Meteors, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Mars Aeronomy, Rings and Dust, Mars, Meteoric metals, Ablation, Planetary Ionospheres, Planetary Geochemistry, Planetary Mineralogy and Petrology, Geochemistry, Ionospheres, Planetary Sciences: Solar System Objects, Mars mesospheric clouds, Mars magnesium layer, Ionosphere, [CHIM.OTHE]Chemical Sciences/Other, Planetary Sciences: Solid Surface Planets, Research Articles, Cosmic dust, Mineralogy and Petrology, Composition, Research Article
Abstract

Recent measurements by the Imaging Ultraviolet Spectrograph (IUVS) instrument on NASA's Mars Atmosphere and Volatile EvolutioN mission show that a persistent layer of Mg+ ions occurs around 90 km in the Martian atmosphere but that neutral Mg atoms are not detectable. These observations can be satisfactorily modeled with a global meteoric ablation rate of 0.06 t sol−1, out of a cosmic dust input of 2.7 ± 1.6 t sol−1. The absence of detectable Mg at 90 km requires that at least 50% of the ablating Mg atoms ionize through hyperthermal collisions with CO2 molecules. Dissociative recombination of MgO+.(CO2)n cluster ions with electrons to produce MgCO3 directly, rather than MgO, also avoids a buildup of Mg to detectable levels. The meteoric injection rate of Mg, Fe, and other metals—constrained by the IUVS measurements—enables the production rate of metal carbonate molecules (principally MgCO3 and FeCO3) to be determined. These molecules have very large electric dipole moments (11.6 and 9.2 Debye, respectively) and thus form clusters with up to six H2O molecules at temperatures below 150 K. These clusters should then coagulate efficiently, building up metal carbonate‐rich ice particles which can act as nucleating particles for the formation of CO2‐ice clouds. Observable mesospheric clouds are predicted to occur between 65 and 80 km at temperatures below 95 K and above 85 km at temperatures about 5 K colder., Key Points A meteoric input function for Mars is generated by combining a cosmic dust input of ~3 tonnes sol−1 with a chemical ablation modelMAVEN/IUVS observations of Mg+, and a small upper limit for Mg, suggest that around 50% of Mg atoms ionize directly after ablationMgCO3 and FeCO3 form stable H2O clusters which coagulate to metal‐rich ice particles, likely nuclei for clouds in the Martian mesosphere

Published
2018

25. Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time

Author

Jakosky, B.M., primary, Brain, D., additional, Chaffin, M., additional, Curry, S., additional, Deighan, J., additional, Grebowsky, J., additional, Halekas, J., additional, Leblanc, F., additional, Lillis, R., additional, Luhmann, J.G., additional, Andersson, L., additional, Andre, N., additional, Andrews, D., additional, Baird, D., additional, Baker, D., additional, Bell, J., additional, Benna, M., additional, Bhattacharyya, D., additional, Bougher, S., additional, Bowers, C., additional, Chamberlin, P., additional, Chaufray, J.-Y., additional, Clarke, J., additional, Collinson, G., additional, Combi, M., additional, Connerney, J., additional, Connour, K., additional, Correira, J., additional, Crabb, K., additional, Crary, F., additional, Cravens, T., additional, Crismani, M., additional, Delory, G., additional, Dewey, R., additional, DiBraccio, G., additional, Dong, C., additional, Dong, Y., additional, Dunn, P., additional, Egan, H., additional, Elrod, M., additional, England, S., additional, Eparvier, F., additional, Ergun, R., additional, Eriksson, A., additional, Esman, T., additional, Espley, J., additional, Evans, S., additional, Fallows, K., additional, Fang, X., additional, Fillingim, M., additional, Flynn, C., additional, Fogle, A., additional, Fowler, C., additional, Fox, J., additional, Fujimoto, M., additional, Garnier, P., additional, Girazian, Z., additional, Groeller, H., additional, Gruesbeck, J., additional, Hamil, O., additional, Hanley, K.G., additional, Hara, T., additional, Harada, Y., additional, Hermann, J., additional, Holmberg, M., additional, Holsclaw, G., additional, Houston, S., additional, Inui, S., additional, Jain, S., additional, Jolitz, R., additional, Kotova, A., additional, Kuroda, T., additional, Larson, D., additional, Lee, Y., additional, Lee, C., additional, Lefevre, F., additional, Lentz, C., additional, Lo, D., additional, Lugo, R., additional, Ma, Y.-J., additional, Mahaffy, P., additional, Marquette, M.L., additional, Matsumoto, Y., additional, Mayyasi, M., additional, Mazelle, C., additional, McClintock, W., additional, McFadden, J., additional, Medvedev, A., additional, Mendillo, M., additional, Meziane, K., additional, Milby, Z., additional, Mitchell, D., additional, Modolo, R., additional, Montmessin, F., additional, Nagy, A., additional, Nakagawa, H., additional, Narvaez, C., additional, Olsen, K., additional, Pawlowski, D., additional, Peterson, W., additional, Rahmati, A., additional, Roeten, K., additional, Romanelli, N., additional, Ruhunusiri, S., additional, Russell, C., additional, Sakai, S., additional, Schneider, N., additional, Seki, K., additional, Sharrar, R., additional, Shaver, S., additional, Siskind, D.E., additional, Slipski, M., additional, Soobiah, Y., additional, Steckiewicz, M., additional, Stevens, M.H., additional, Stewart, I., additional, Stiepen, A., additional, Stone, S., additional, Tenishev, V., additional, Terada, N., additional, Terada, K., additional, Thiemann, E., additional, Tolson, R., additional, Toth, G., additional, Trovato, J., additional, Vogt, M., additional, Weber, T., additional, Withers, P., additional, Xu, S., additional, Yelle, R., additional, Yiğit, E., additional, and Zurek, R., additional

Published
2018
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27. Martian Thermospheric Response to an X8.2 Solar Flare on 10 September 2017 as Seen by MAVEN/IUVS

Author

Jain, S. K., primary, Deighan, J., additional, Schneider, N. M., additional, Stewart, A. I. F., additional, Evans, J. S., additional, Thiemann, E. M. B., additional, Chaffin, M. S., additional, Crismani, M., additional, Stevens, M. H., additional, Elrod, M. K., additional, Stiepen, A., additional, McClintock, W. E., additional, Lo, D. Y., additional, Clarke, J. T., additional, Eparvier, F. G., additional, Lefévre, F., additional, Montmessin, F., additional, Holsclaw, G. M., additional, Chamberlin, P. C., additional, and Jakosky, B. M., additional

Published
2018
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28. Global Aurora on Mars During the September 2017 Space Weather Event

Author

Schneider, N. M., primary, Jain, S. K., additional, Deighan, J., additional, Nasr, C. R., additional, Brain, D. A., additional, Larson, D., additional, Lillis, R., additional, Rahmati, Ali, additional, Halekas, J. S., additional, Lee, C. O., additional, Chaffin, M. S., additional, Stiepen, A., additional, Crismani, M., additional, Evans, J. S., additional, Stevens, M. H., additional, Lo, D. Y., additional, McClintock, W. E., additional, Stewart, A. I. F., additional, Yelle, R. V., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Lefevre, F., additional, Montmessin, F., additional, and Jakosky, B. M., additional

Published
2018
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29. Mars H Escape Rates Derived From MAVEN/IUVS Lyman Alpha Brightness Measurements and Their Dependence on Model Assumptions

Author

Chaffin, M. S., primary, Chaufray, J. Y., additional, Deighan, J., additional, Schneider, N. M., additional, Mayyasi, M., additional, Clarke, J. T., additional, Thiemann, E., additional, Jain, S. K., additional, Crismani, M. M. J., additional, Stiepen, A., additional, Eparvier, F. G., additional, McClintock, W. E., additional, Stewart, A. I. F., additional, Holsclaw, G. M., additional, Montmessin, F., additional, and Jakosky, B. M., additional

Published
2018
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30. Martian mesospheric cloud observations by IUVS on MAVEN: Thermal tides coupled to the upper atmosphere

Author

Stevens, M. H., primary, Siskind, D. E., additional, Evans, J. S., additional, Jain, S. K., additional, Schneider, N. M., additional, Deighan, J., additional, Stewart, A. I. F., additional, Crismani, M., additional, Stiepen, A., additional, Chaffin, M. S., additional, McClintock, W. E., additional, Holsclaw, G. M., additional, Lefèvre, F., additional, Lo, D. Y., additional, Clarke, J. T., additional, Montmessin, F., additional, and Jakosky, B. M., additional

Published
2017
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31. Detection of a persistent meteoric metal layer in the Martian atmosphere

Author

Crismani, M. M. J., primary, Schneider, N. M., additional, Plane, J. M. C., additional, Evans, J. S., additional, Jain, S. K., additional, Chaffin, M. S., additional, Carrillo-Sanchez, J. D., additional, Deighan, J. I., additional, Yelle, R. V., additional, Stewart, A. I. F., additional, McClintock, W., additional, Clarke, J., additional, Holsclaw, G. M., additional, Stiepen, A., additional, Montmessin, F., additional, and Jakosky, B. M., additional

Published
2017
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32. Nitric oxide nightglow and Martian mesospheric circulation from MAVEN/IUVS observations and LMD‐MGCM predictions

Author

Stiepen, A., primary, Jain, S. K., additional, Schneider, N. M., additional, Deighan, J. I., additional, González‐Galindo, F., additional, Gérard, J.‐C., additional, Milby, Z., additional, Stevens, M. H., additional, Bougher, S., additional, Evans, J. S., additional, Stewart, A. I. F., additional, Chaffin, M. S., additional, Crismani, M., additional, McClintock, W. E., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Montmessin, F., additional, Lefèvre, F., additional, Forget, F., additional, Lo, D. Y., additional, Hubert, B., additional, and Jakosky, B. M., additional

Published
2017
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33. Variability of D and H in the Martian upper atmosphere observed with the MAVEN IUVS echelle channel

Author

Clarke, J. T., primary, Mayyasi, M., additional, Bhattacharyya, D., additional, Schneider, N. M., additional, McClintock, W. E., additional, Deighan, J. I., additional, Stewart, A. I. F., additional, Chaufray, J.‐Y., additional, Chaffin, M. S., additional, Jain, S. K., additional, Stiepen, A., additional, Crismani, M., additional, Holsclaw, G. M., additional, Montmessin, F., additional, and Jakosky, B. M., additional

Published
2017
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34. Localized Ionization Hypothesis for Transient Ionospheric Layers.

Author

Deighan, J., Schneider, N. M., Chaffin, M., Jain, S., Crismani, M. M. J., Plane, J. M. C., Withers, P., and Halekas, J.

Subjects
MARTIAN ionosphere, ULTRAVIOLET radiation, IONIZATION (Atomic physics), METEORS, ABLATION (Aerothermodynamics), REMOTE sensing, SOLAR wind, IONS
Abstract

The persistent two‐peaked vertical structure of the Martian ionosphere is created by extreme and far ultraviolet radiation whose energies, respectively, determine their ionization altitude. A third low‐altitude transient layer (previously referred to as M3 or Mm) has been observed by radio occultation techniques and attributed to meteor ablation. However, recent remote sensing and in situ observations disfavor a meteoric origin. Here we propose an alternative hypothesis for these apparent layers associated with impact ionization from penetrating solar wind ions, previously observed as proton aurora. Localized ionization, occurring nonglobally at a given altitude range, breaks the symmetry assumed by the radio occultation technique, and creates electron layers apparently lower in the ionosphere than their true altitude. This may occur when the upstream bow shock is altered by a radial interplanetary magnetic field configuration, which allows the solar wind to penetrate directly into the thermosphere. This localized ionization hypothesis provides an explanation for apparent layers' wide variation in heights and their transient behavior. Moreover, this hypothesis is testable with new observations by the Mars Atmospheric and Volatile EvolutioN Radio Occultation Science Experiment in future Mars years. This hypothesis has implications for the ionospheres of Venus and Titan, where similar transient layers have been observed. Plain Language Summary: The ionosphere of a planet couples the neutral atmosphere to the exosphere and solar wind. Created by solar ionizing radiation, the ionosphere on the dayside of planet is expected to be hemispherically symmetric. When Mars Express discovered transient low‐altitude ionospheric layers in 2005, they were initially predicted to be due to meteor ablation. However, recent observations indicate that they are due to a geometric observational effect related to local, not hemispheric, ionization. Observations from three instruments on Mars Atmospheric and Volatile EvolutioN are used concurrently to understand this phenomenon. These transient layers have been observed at Venus and Titan as well, and this hypothesis indicates novel physics for those ionospheric systems. Key Points: Low‐altitude transient ionospheric layers may be explained by a geometric observational effect from localized, not hemispheric, ionizationA radio occultation of a transient ionospheric layer was obtained with observations of variable proton aurora and penetrating solar windTransient layers observed at Mars, Venus, and Titan are consistent with the presence of solar wind impact ionization at those planets [ABSTRACT FROM AUTHOR]

Published
2019
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35. Probing the Martian atmosphere with MAVEN/IUVS stellar occultations

Author

Gröller, H., primary, Yelle, R. V., additional, Koskinen, T. T., additional, Montmessin, F., additional, Lacombe, G., additional, Schneider, N. M., additional, Deighan, J., additional, Stewart, A. I. F., additional, Jain, S. K., additional, Chaffin, M. S., additional, Crismani, M. M. J., additional, Stiepen, A., additional, Lefèvre, F., additional, McClintock, W. E., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Mahaffy, P. R., additional, Bougher, S. W., additional, and Jakosky, B. M., additional

Published
2015
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36. The structure and variability of Mars upper atmosphere as seen in MAVEN/IUVS dayglow observations

Author

Jain, S. K., primary, Stewart, A. I. F., additional, Schneider, N. M., additional, Deighan, J., additional, Stiepen, A., additional, Evans, J. S., additional, Stevens, M. H., additional, Chaffin, M. S., additional, Crismani, M., additional, McClintock, W. E., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Lo, D. Y., additional, Lefèvre, F., additional, Montmessin, F., additional, Thiemann, E. M. B., additional, Eparvier, F., additional, and Jakosky, B. M., additional

Published
2015
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37. Retrieval of CO2 and N2 in the Martian thermosphere using dayglow observations by IUVS on MAVEN

Author

Evans, J. S., primary, Stevens, M. H., additional, Lumpe, J. D., additional, Schneider, N. M., additional, Stewart, A. I. F., additional, Deighan, J., additional, Jain, S. K., additional, Chaffin, M. S., additional, Crismani, M., additional, Stiepen, A., additional, McClintock, W. E., additional, Holsclaw, G. M., additional, Lefèvre, F., additional, Lo, D. Y., additional, Clarke, J. T., additional, Eparvier, F. G., additional, Thiemann, E. M. B., additional, Chamberlin, P. C., additional, Bougher, S. W., additional, Bell, J. M., additional, and Jakosky, B. M., additional

Published
2015
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38. Three‐dimensional structure in the Mars H corona revealed by IUVS on MAVEN

Author

Chaffin, M. S., primary, Chaufray, J. Y., additional, Deighan, J., additional, Schneider, N. M., additional, McClintock, W. E., additional, Stewart, A. I. F., additional, Thiemann, E., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Jain, S. K., additional, Crismani, M. M. J., additional, Stiepen, A., additional, Montmessin, F., additional, Eparvier, F. G., additional, Chamberlain, P. C., additional, and Jakosky, B. M., additional

Published
2015
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39. Study of the Martian cold oxygen corona from the O I 130.4 nm by IUVS/MAVEN

Author

Chaufray, J. Y., primary, Deighan, J., additional, Chaffin, M. S., additional, Schneider, N. M., additional, McClintock, W. E., additional, Stewart, A. I. F., additional, Jain, S. K., additional, Crismani, M., additional, Stiepen, A., additional, Holsclaw, G. M., additional, Clarke, J. T., additional, Montmessin, F., additional, Eparvier, F. G., additional, Thiemann, E. M. B., additional, Chamberlin, P. C., additional, and Jakosky, B. M., additional

Published
2015
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40. New observations of molecular nitrogen in the Martian upper atmosphere by IUVS on MAVEN

Author

Stevens, M. H., primary, Evans, J. S., additional, Schneider, N. M., additional, Stewart, A. I. F., additional, Deighan, J., additional, Jain, S. K., additional, Crismani, M., additional, Stiepen, A., additional, Chaffin, M. S., additional, McClintock, W. E., additional, Holsclaw, G. M., additional, Lefèvre, F., additional, Lo, D. Y., additional, Clarke, J. T., additional, Montmessin, F., additional, Bougher, S. W., additional, and Jakosky, B. M., additional

Published
2015
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41. MAVEN IUVS observation of the hot oxygen corona at Mars

Author

Deighan, J., primary, Chaffin, M. S., additional, Chaufray, J.‐Y., additional, Stewart, A. I. F., additional, Schneider, N. M., additional, Jain, S. K., additional, Stiepen, A., additional, Crismani, M., additional, McClintock, W. E., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Montmessin, F., additional, Eparvier, F. G., additional, Thiemann, E. M. B., additional, Chamberlin, P. C., additional, and Jakosky, B. M., additional

Published
2015
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42. MAVEN IUVS observations of the aftermath of the Comet Siding Spring meteor shower on Mars

Author

Schneider, N. M., primary, Deighan, J. I., additional, Stewart, A. I. F., additional, McClintock, W. E., additional, Jain, S. K., additional, Chaffin, M. S., additional, Stiepen, A., additional, Crismani, M., additional, Plane, J. M. C., additional, Carrillo‐Sánchez, J. D., additional, Evans, J. S., additional, Stevens, M. H., additional, Yelle, R. V., additional, Clarke, J. T., additional, Holsclaw, G. M., additional, Montmessin, F., additional, and Jakosky, B. M., additional

Published
2015
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45. Martian Meteoric Mg+: Atmospheric Distribution and Variability From MAVEN/IUVS

Author

Crismani, M. M. J., Tyo, R. M., Schneider, N. M., Plane, J. M. C., Feng, W., Carrillo‐Sánchez, J. D., Villanueva, G. L., Jain, S., Deighan, J., and Curry, S.

Abstract

Since the discovery of atmospheric Mg+on Mars in 2015 by the Mars Atmosphere and Volatile Evolution mission, there have been almost continuous observations of this meteoric ion layer in a variety of seasons, local times, and latitudes. Here, we present the most comprehensive set of observations of the persistent metal ion layer at Mars, constructing the first grand composite maps from pooled medians of subsamples of a metallic ion species. These maps demonstrate that Mg+appears in almost all conditions when illuminated, with peak density values varying between 100 and 500 cm−3, dependent on season and local time. There exists significant latitudinal variation within a given season, indicating that Mg+is not simply an inert tracer, but may instead be influenced by the meteoric input distribution and/or atmospheric dynamics and chemistry. Geographic maps of Mg+density as a function of latitude and longitude indicate the influence of atmospheric tides, and there is no apparent correlation with remnant crustal magnetic fields. This work also presents counter‐intuitive results, such as a reduction of Mg+ions in the northern hemisphere during Northern Winter in an apparent correlation with dust aerosols. Metallic atoms in a planet's atmosphere are present when interplanetary dust particles burn up, releasing atomic species not typically found in the lower atmosphere. The discovery of a high altitude metallic layer on Mars in 2015 has led to continued monitoring in a variety of seasons across the entire planet. These results demonstrate that this magnesium ion (Mg+) layer appears throughout the year, with variations in peak abundances and layer heights, due to interactions with the background atmosphere. These variations track the dynamics of the middle atmosphere, providing insight into global climate patterns and may inform our understanding of seasonal deposition of interplanetary dust particles and their sources. This first‐order analysis supports future modeling efforts and provides model challenges to be understood, both of which can be explored in detail with time varying full planet climate modeling. Eight Earth years of Mars Atmosphere and Volatile Evolution/Imaging Ultraviolet Spectrograph observations show that Mars' persistent meteoric metal ion layer is more dynamic than initially assumedMg+layer peak altitude, abundance, and top and bottom side slopes vary significantly over the observed time periodThe relative absence of northern hemispheric Mg+during southern summer is surprising and may be related to lower atmospheric dust loading Eight Earth years of Mars Atmosphere and Volatile Evolution/Imaging Ultraviolet Spectrograph observations show that Mars' persistent meteoric metal ion layer is more dynamic than initially assumed Mg+layer peak altitude, abundance, and top and bottom side slopes vary significantly over the observed time period The relative absence of northern hemispheric Mg+during southern summer is surprising and may be related to lower atmospheric dust loading

Published
2023
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47. Retrieval of CO2and N2in the Martian thermosphere using dayglow observations by IUVS on MAVEN

Author

Evans, J. S., Stevens, M. H., Lumpe, J. D., Schneider, N. M., Stewart, A. I. F., Deighan, J., Jain, S. K., Chaffin, M. S., Crismani, M., Stiepen, A., McClintock, W. E., Holsclaw, G. M., Lefèvre, F., Lo, D. Y., Clarke, J. T., Eparvier, F. G., Thiemann, E. M. B., Chamberlin, P. C., Bougher, S. W., Bell, J. M., and Jakosky, B. M.

Abstract

We present direct number density retrievals of carbon dioxide (CO2) and molecular nitrogen (N2) for the upper atmosphere of Mars using limb scan observations during October and November 2014 by the Imaging Ultraviolet Spectrograph on board NASA's Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. We use retrieved CO2densities to derive temperature variability between 170 and 220 km. Analysis of the data shows (1) low‐mid latitude northern hemisphere CO2densities at 170 km vary by a factor of about 2.5, (2) on average, the N2/CO2increases from 0.042 ± 0.017 at 130 km to 0.12 ± 0.06 at 200 km, and (3) the mean upper atmospheric temperature is 324 ± 22 K for local times near 14:00. Retrieved CO2densities at 170 km vary by a factor of about 2.5On average, N2/CO2increases from 4% at 130 km to 12% at 200 kmMean Martian upper atmospheric temperature over the sampled time frame is 324 {±} 22 K

Published
2015
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48. Maps of Martian Atmospheric H2O with Trace Gas Orbiter's NOMAD/LNO.

Author

Crismani, M. M. J., Villanueva, G., Liuzzi, G., Mumma, M. J., Smith, M. D., Vandaele, A. C., Aoki, S., Thomas, I. R., Daerden, F., Lopez-Valverde, M. A., Ristic, B., Patel, M. R., Bellucci, G., and Lopez Moren4, J-J

Subjects
TRACE gases, MARTIAN atmosphere, WATER, GENERAL circulation model, FOCAL plane arrays sensors, LATITUDE
Published
2019

49. A Global and Seasonal Perspective of Martian Water Vapor from ExoMars/NOMAD

Author

Crismani, M. M. J., Villanueva, G. L., Liuzzi, G., Smith, M. D., Knutsen, E. W., Daerden, F., Neary, L., Mumma, M. J., Aoki, S., Trompet, L., Thomas, I.R., Ristic, B., Bellucci, G., Piccialli, A., Robert, S., Mahieux, A., Lopez Moreno, J‐J, Sindoni, G., Giuranna, M., Patel, M. R, Vandaele, A. C., Crismani, M. M. J., Villanueva, G. L., Liuzzi, G., Smith, M. D., Knutsen, E. W., Daerden, F., Neary, L., Mumma, M. J., Aoki, S., Trompet, L., Thomas, I.R., Ristic, B., Bellucci, G., Piccialli, A., Robert, S., Mahieux, A., Lopez Moreno, J‐J, Sindoni, G., Giuranna, M., Patel, M. R, and Vandaele, A. C.

Abstract

Slightly less than a Martian Year of nominal science (March 2018–January 2020) with the ExoMars Trace Gas Orbiter has furthered the ongoing investigation of dayside water vapor column abundance. These dayside observations span latitudes between 75°S and 75°N, and all longitudes, which can provide global snapshots of the total water column abundances. In addition to tracking the seasonal transport of water vapor between poles, geographic enhancements are noted, particularly in the southern hemisphere, both in Hellas Basin, and in other regions not obviously correlated to topography. We report consistent water vapor climatology with previous spacecraft observations, however, note a difference in total water vapor content is noted. Finally, we are unable to find evidence for substantial diurnal variation in the total dayside water vapor column.

50. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

Author

Aoki, S., Daerden, F., Viscardy, S., Thomas, I. R., Erwin, J. T., Robert, S., Trompet, L., Neary, L., Villanueva, G. L., Liuzzi, G., Crismani, M. M. J., Clancy, R. T., Whiteway, J., Schmidt, F., Lopez‐Valverde, M. A., Ristic, B., Patel, M.R., Bellucci, G., Lopez‐Moreno, J.‐J., Olsen, K. S., Lefèvre, F., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Korablev, O., Vandaele, A. C., Aoki, S., Daerden, F., Viscardy, S., Thomas, I. R., Erwin, J. T., Robert, S., Trompet, L., Neary, L., Villanueva, G. L., Liuzzi, G., Crismani, M. M. J., Clancy, R. T., Whiteway, J., Schmidt, F., Lopez‐Valverde, M. A., Ristic, B., Patel, M.R., Bellucci, G., Lopez‐Moreno, J.‐J., Olsen, K. S., Lefèvre, F., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Korablev, O., and Vandaele, A. C.

Abstract

Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. The reported detection made in Martian Year 34 was transient, present several months after the global dust storm during the southern summer season. Here, we present the full data set of vertically resolved HCl detections obtained by the NOMAD instrument, which covers also Martian year 35. We show that the particular increase of HCl abundances in the southern summer season is annually repeated, and that the formation of HCl is independent from a global dust storm event. We also find that the vertical distribution of HCl is strikingly similar to that of water vapor, which suggests that the uptake by water ice clouds plays an important role. The observed rapid decrease of HCl abundances at the end of the southern summer would require a strong sink independent of photochemical loss.

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