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Sánchez‐Lavega A, del Rio‐Gaztelurrutia T, Hueso R, Juárez MDLT, Martínez GM, Harri A, Genzer M, Hieta M, Polkko J, Rodríguez‐Manfredi JA, Lemmon MT, Pla‐García J, Toledo D, Vicente‐Retortillo A, Viúdez‐Moreiras D, Munguira A, Tamppari LK, Newman C, Gómez‐Elvira J, Guzewich S, Bertrand T, Apéstigue V, Arruego I, Wolff M, Banfield D, Jaakonaho I, Mäkinen T. Mars 2020 Perseverance Rover Studies of the Martian Atmosphere Over Jezero From Pressure Measurements. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2023; 128:e2022JE007480. [PMID: 37034458 PMCID: PMC10078360 DOI: 10.1029/2022je007480] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/10/2022] [Revised: 10/05/2022] [Accepted: 10/24/2022] [Indexed: 06/16/2023]
Abstract
The pressure sensors on Mars rover Perseverance measure the pressure field in the Jezero crater on regular hourly basis starting in sol 15 after landing. The present study extends up to sol 460 encompassing the range of solar longitudes from L s ∼ 13°-241° (Martian Year (MY) 36). The data show the changing daily pressure cycle, the sol-to-sol seasonal evolution of the mean pressure field driven by the CO2 sublimation and deposition cycle at the poles, the characterization of up to six components of the atmospheric tides and their relationship to dust content in the atmosphere. They also show the presence of wave disturbances with periods 2-5 sols, exploring their baroclinic nature, short period oscillations (mainly at night-time) in the range 8-24 min that we interpret as internal gravity waves, transient pressure drops with duration ∼1-150 s produced by vortices, and rapid turbulent fluctuations. We also analyze the effects on pressure measurements produced by a regional dust storm over Jezero at L s ∼ 155°.
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Affiliation(s)
| | | | | | | | | | - A.‐M. Harri
- Finnish Meteorological InstituteHelsinkiFinland
| | - M. Genzer
- Finnish Meteorological InstituteHelsinkiFinland
| | - M. Hieta
- Finnish Meteorological InstituteHelsinkiFinland
| | - J. Polkko
- Finnish Meteorological InstituteHelsinkiFinland
| | | | | | | | - D. Toledo
- Centro de Astrobiología (INTA‐CSIC)MadridSpain
| | | | | | | | - L. K. Tamppari
- Jet Propulsion Laboratory/California Institute of TechnologyPasadenaCAUSA
| | | | | | - S. Guzewich
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | | | - V. Apéstigue
- Instituto Nacional de Técnica AeroespacialINTAMadridSpain
| | - I. Arruego
- Instituto Nacional de Técnica AeroespacialINTAMadridSpain
| | - M. Wolff
- Space Science InstituteBrookfieldWIUSA
| | | | | | - T. Mäkinen
- Finnish Meteorological InstituteHelsinkiFinland
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Lange L, Forget F, Banfield D, Wolff M, Spiga A, Millour E, Viúdez‐Moreiras D, Bierjon A, Piqueux S, Newman C, Pla‐García J, Banerdt WB. InSight Pressure Data Recalibration, and Its Application to the Study of Long-Term Pressure Changes on Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2022JE007190. [PMID: 35865505 PMCID: PMC9286347 DOI: 10.1029/2022je007190] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 01/15/2022] [Revised: 05/09/2022] [Accepted: 05/12/2022] [Indexed: 06/15/2023]
Abstract
Observations of the South Polar Residual Cap suggest a possible erosion of the cap, leading to an increase of the global mass of the atmosphere. We test this assumption by making the first comparison between Viking 1 and InSight surface pressure data, which were recorded 40 years apart. Such a comparison also allows us to determine changes in the dynamics of the seasonal ice caps between these two periods. To do so, we first had to recalibrate the InSight pressure data because of their unexpected sensitivity to the sensor temperature. Then, we had to design a procedure to compare distant pressure measurements. We propose two surface pressure interpolation methods at the local and global scale to do the comparison. The comparison of Viking and InSight seasonal surface pressure variations does not show changes larger than ±8 Pa in the CO2 cycle. Such conclusions are supported by an analysis of Mars Science Laboratory (MSL) pressure data. Further comparisons with images of the south seasonal cap taken by the Viking 2 orbiter and MARCI camera do not display significant changes in the dynamics of this cap over a 40 year period. Only a possible larger extension of the North Cap after the global storm of MY 34 is observed, but the physical mechanisms behind this anomaly are not well determined. Finally, the first comparison of MSL and InSight pressure data suggests a pressure deficit at Gale crater during southern summer, possibly resulting from a large presence of dust suspended within the crater.
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Affiliation(s)
- L. Lange
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - F. Forget
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - D. Banfield
- Cornell Center for Astrophysics and Planetary ScienceCornell UniversityIthacaNYUSA
| | - M. Wolff
- Space Science InstituteBoulderCOUSA
| | - A. Spiga
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
- Institut Universitaire de FranceParisFrance
| | - E. Millour
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - D. Viúdez‐Moreiras
- Centro de Astrobiología (CSIC‐INTA) and National Institute for Aerospace Technology (INTA)MadridSpain
| | - A. Bierjon
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - S. Piqueux
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - J. Pla‐García
- Centro de Astrobiología (CSIC‐INTA) and National Institute for Aerospace Technology (INTA)MadridSpain
- Southwest Research InstituteBoulderCOUSA
| | - W. B. Banerdt
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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Hinson DP, Wilson RJ. Baroclinic waves in the northern hemisphere of Mars as observed by the MRO Mars Climate Sounder and the MGS Thermal Emission Spectrometer. ICARUS 2021; 357:114152. [PMID: 34646052 PMCID: PMC8506978 DOI: 10.1016/j.icarus.2020.114152] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
The climatology of baroclinic waves in the northern hemisphere of Mars is investigated through analysis of observations by the infrared sounders on Mars Reconnaissance Orbiter (MRO) and Mars Global Surveyor (MGS). We focus on the lowest scale height above the surface, where the waves have a large impact on the Martian dust cycle. Profiles retrieved by the MRO Mars Climate Sounder (MCS) rarely reach the lower atmosphere at the season and location of interest. To fill this gap, we turn to observations in the MCS B1 channel (32 microns) when the instrument is viewing the surface. The signature of baroclinic waves appears in these data because of dust-related emission from the lower atmosphere and wave-induced variations of surface temperature. We supplement the MCS data with measurements of temperature at the 610-Pa pressure level from the MGS Thermal Emission Spectrometer (TES). Both data sets provide systematic coverage in latitude and longitude at two local times. Characteristics of baroclinic waves are derived through analysis of observations with a combined duration of about 8 Mars years. Basic results include least-squares solutions for wave amplitude and period at zonal wavenumber 1-3; the resolution is 4° in latitude and 14 solar days in time of observation. There is a strong similarity between the baroclinic waves observed by MCS and TES, which confirms the sensitivity of the MCS B1 channel to wave activity at pressures near 610 Pa. In all 8 Mars years, the baroclinic waves exhibit periodic transitions among modes with different zonal wavenumbers and a distinctive solstitial pause. Although the weather in each Mars year is unique in some respects, a composite of results from all years reveals a well-defined wave climatology. At each zonal wavenumber, large amplitudes are restricted to a pair of seasonal windows positioned symmetrically about the winter solstice. The wave-2 mode is strongest in early autumn and near the vernal equinox, whereas wave 3 is the dominant mode in mid-autumn and mid-winter, immediately before and after the solstitial pause. The interaction between baroclinic waves and dust storms is investigated through comparisons with spacecraft measurements of dust opacity. A strong wave-3 mode is often present during the initial growth phase of large, seasonal dust storms, which reflects the importance of wave-generated frontal dust storms in triggering these events. The wave-3 amplitude then decreases rapidly as the dust storm evolves; this occurs routinely in all Mars years considered here in connection with both mid-autumn "A" storms and mid-winter "C" storms. In some years A-storm suppression of the wave-3 mode marks the beginning of the solstitial pause. These results provide a basis for testing and development of Mars General Circulation Models as well as context for interpreting contemporaneous observations, such as spacecraft images of frontal and flushing dust storms.
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Affiliation(s)
- David P. Hinson
- Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA
| | - R. John Wilson
- Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, CA 94035, USA
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Viúdez-Moreiras D, Newman CE, de la Torre M, Martínez G, Guzewich S, Lemmon M, Pla-García J, Smith MD, Harri AM, Genzer M, Vicente-Retortillo A, Lepinette A, Rodriguez-Manfredi JA, Vasavada AR, Gómez-Elvira J. Effects of the MY34/2018 Global Dust Storm as Measured by MSL REMS in Gale Crater. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2019; 124:1899-1912. [PMID: 31534881 PMCID: PMC6750032 DOI: 10.1029/2019je005985] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/29/2019] [Accepted: 06/19/2019] [Indexed: 05/28/2023]
Abstract
The Rover Environmental Monitoring Station (REMS) instrument that is onboard NASA's Mars Science Laboratory (MSL) Curiosity rover. REMS has been measuring surface pressure, air and ground brightness temperature, relative humidity, and UV irradiance since MSL's landing in 2012. In Mars Year (MY) 34 (2018) a global dust storm reached Gale Crater at Ls ~190°. REMS offers a unique opportunity to better understand the impact of a global dust storm on local environmental conditions, which complements previous observations by the Viking landers and Mars Exploration Rovers. All atmospheric variables measured by REMS are strongly affected albeit at different times. During the onset phase, the daily maximum UV radiation decreased by 90% between sols 2075 (opacity ~1) and 2085 (opacity ~8.5). The diurnal range in ground and air temperatures decreased by 35K and 56K, respectively, with also a diurnal-average decrease of ~2K and 4K respectively. The maximum relative humidity, which occurs right before sunrise, decreased to below 5%, compared with pre-storm values of up to 29%, due to the warmer air temperatures at night while the inferred water vapor abundance suggests an increase during the storm. Between sols 2085 and 2130, the typical nighttime stable inversion layer was absent near the surface as ground temperatures remained warmer than near-surface air temperatures. Finally, the frequency-domain behavior of the diurnal pressure cycle shows a strong increase in the strength of the semidiurnal and terdiurnal modes peaking after the local opacity maximum, also suggesting differences in the dust abundance inside and outside Gale.
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Affiliation(s)
- D Viúdez-Moreiras
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - C E Newman
- Aeolis Research, 600 N. Rosemead Ave., Suite 205, Pasadena, CA 91106, USA
| | - M de la Torre
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - G Martínez
- University of Michigan, Ann Arbor, Michigan, USA
| | - S Guzewich
- NASA Goddard Spaceflight Center, Greenbelt, MD, USA
| | - M Lemmon
- Space Science Institute, College Station, TX 77843 USA
| | - J Pla-García
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - M D Smith
- NASA Goddard Spaceflight Center, Greenbelt, MD, USA
| | - A-M Harri
- Earth Observation, Finnish Meteorological Institute, Erik Palménin aukio, Helsinki, Finland
| | - M Genzer
- Earth Observation, Finnish Meteorological Institute, Erik Palménin aukio, Helsinki, Finland
| | | | - A Lepinette
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - J A Rodriguez-Manfredi
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - A R Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - J Gómez-Elvira
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
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Zurek RW, Martin LJ. Interannual variability of planet-encircling dust storms on Mars. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92je02936] [Citation(s) in RCA: 132] [Impact Index Per Article: 11.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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7
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Hinson DP. Radio occultation measurements of transient eddies in the northern hemisphere of Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002612] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Murphy JR, Leovy CB, Tillman JE. Observations of Martian surface winds at the Viking Lander 1 Site. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14555] [Citation(s) in RCA: 58] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Arvidson RE, Guinness EA, Moore HJ, Tillman J, Wall SD. Three Mars Years: Viking Lander 1 Imaging Observations. Science 1983; 222:463-8. [PMID: 17746178 DOI: 10.1126/science.222.4623.463] [Citation(s) in RCA: 94] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Mutch Memorial Station (Viking Lander 1) on Mars acquired imaging and meteorological data over a period of 2245 martian days (3:3 martian years). This article discusses the deposition and erosion of thin deposits (ten to hundreds of micrometers) of bright red dust associated with global dust storms, and the removal of centimeter amounts of material in selected areas during a dust storm late in the third winter. Atmospheric pressure data acquired during the period of intense erosion imply that baroclinic disturbances and strong diurnal solar tidal heating combined to produce strong winds. Erosion occurred principally in areas where soil cohesion was reduced by earlier surface sampler activities. Except for redistribution of thin layers of materials, the surface appears to be remarkably stable, perhaps because of cohesion of the undisturbed surface material.
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11
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12
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James PB, North GR. The seasonal CO2cycle on Mars: An application of an energy balance climate model. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10271] [Citation(s) in RCA: 59] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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13
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Niver DS, Hess SL. Band-pass filtering of one year of daily mean pressures on Mars. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10191] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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