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Brinkman N, Schmelzbach C, Sollberger D, Pierick JT, Edme P, Haag T, Kedar S, Hudson T, Andersson F, van Driel M, Stähler S, Nicollier T, Robertsson J, Giardini D, Spohn T, Krause C, Grott M, Knollenberg J, Hurst K, Rochas L, Vallade J, Blandin S, Lognonné P, Pike WT, Banerdt WB. In Situ Regolith Seismic Velocity Measurement at the InSight Landing Site on Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2022JE007229. [PMID: 36582924 PMCID: PMC9787532 DOI: 10.1029/2022je007229] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 02/02/2022] [Revised: 07/15/2022] [Accepted: 09/15/2022] [Indexed: 06/17/2023]
Abstract
Interior exploration using Seismic Investigations, Geodesy and Heat Transport's (InSight) seismometer package Seismic Experiment for Interior Structure (SEIS) was placed on the surface of Mars at about 1.2 m distance from the thermal properties instrument Heat flow and Physical Properties Package (HP3) that includes a self-hammering probe. Recording the hammering noise with SEIS provided a unique opportunity to estimate the seismic wave velocities of the shallow regolith at the landing site. However, the value of studying the seismic signals of the hammering was only realized after critical hardware decisions were already taken. Furthermore, the design and nominal operation of both SEIS and HP3 are nonideal for such high-resolution seismic measurements. Therefore, a series of adaptations had to be implemented to operate the self-hammering probe as a controlled seismic source and SEIS as a high-frequency seismic receiver including the design of a high-precision timing and an innovative high-frequency sampling workflow. By interpreting the first-arriving seismic waves as a P-wave and identifying first-arriving S-waves by polarization analysis, we determined effective P- and S-wave velocities of v P = 11 9 - 21 + 45 m/s and v S = 6 3 - 7 + 11 m/s, respectively, from around 2,000 hammer stroke recordings. These velocities likely represent bulk estimates for the uppermost several 10s of cm of regolith. An analysis of the P-wave incidence angles provided an independent v P /v S ratio estimate of 1.8 4 - 0.35 + 0.89 that compares well with the traveltime based estimate of 1.8 6 - 0.25 + 0.42 . The low seismic velocities are consistent with those observed for low-density unconsolidated sands and are in agreement with estimates obtained by other methods.
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Affiliation(s)
| | | | | | | | - Pascal Edme
- Institute of GeophysicsETH ZürichZürichSwitzerland
| | - Thomas Haag
- Institute of GeophysicsETH ZürichZürichSwitzerland
| | - Sharon Kedar
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Troy Hudson
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | | | | | | | | | - Tilman Spohn
- Deutsches Zentrum für Luft‐ und Raumfahrt (DLR)BremenGermany
- International Space Science InstituteBernSwitzerland
| | | | - Matthias Grott
- Deutsches Zentrum für Luft‐ und Raumfahrt (DLR)BremenGermany
| | | | - Ken Hurst
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Ludovic Rochas
- Centre National des Études Spatiales (CNES)ToulouseFrance
| | - Julien Vallade
- Centre National des Études Spatiales (CNES)ToulouseFrance
| | - Steve Blandin
- Centre National des Études Spatiales (CNES)ToulouseFrance
| | - Philippe Lognonné
- Université Paris CitéInstitut de physique du globe de ParisCNRSParisFrance
| | | | - W. Bruce Banerdt
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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Newman CE, Hueso R, Lemmon MT, Munguira A, Vicente-Retortillo Á, Apestigue V, Martínez GM, Toledo D, Sullivan R, Herkenhoff KE, de la Torre Juárez M, Richardson MI, Stott AE, Murdoch N, Sanchez-Lavega A, Wolff MJ, Arruego I, Sebastián E, Navarro S, Gómez-Elvira J, Tamppari L, Viúdez-Moreiras D, Harri AM, Genzer M, Hieta M, Lorenz RD, Conrad P, Gómez F, McConnochie TH, Mimoun D, Tate C, Bertrand T, Bell JF, Maki JN, Rodriguez-Manfredi JA, Wiens RC, Chide B, Maurice S, Zorzano MP, Mora L, Baker MM, Banfield D, Pla-Garcia J, Beyssac O, Brown A, Clark B, Lepinette A, Montmessin F, Fischer E, Patel P, del Río-Gaztelurrutia T, Fouchet T, Francis R, Guzewich SD. The dynamic atmospheric and aeolian environment of Jezero crater, Mars. SCIENCE ADVANCES 2022; 8:eabn3783. [PMID: 35613267 PMCID: PMC9132482 DOI: 10.1126/sciadv.abn3783] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 11/22/2021] [Accepted: 04/08/2022] [Indexed: 06/15/2023]
Abstract
Despite the importance of sand and dust to Mars geomorphology, weather, and exploration, the processes that move sand and that raise dust to maintain Mars' ubiquitous dust haze and to produce dust storms have not been well quantified in situ, with missions lacking either the necessary sensors or a sufficiently active aeolian environment. Perseverance rover's novel environmental sensors and Jezero crater's dusty environment remedy this. In Perseverance's first 216 sols, four convective vortices raised dust locally, while, on average, four passed the rover daily, over 25% of which were significantly dusty ("dust devils"). More rarely, dust lifting by nonvortex wind gusts was produced by daytime convection cells advected over the crater by strong regional daytime upslope winds, which also control aeolian surface features. One such event covered 10 times more area than the largest dust devil, suggesting that dust devils and wind gusts could raise equal amounts of dust under nonstorm conditions.
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Affiliation(s)
| | | | | | | | | | | | - Germán M. Martínez
- Lunar and Planetary Institute, USRA, Houston, TX, USA
- University of Michigan, Ann Arbor, MI, USA
| | | | | | | | | | | | | | - Naomi Murdoch
- ISAE-SUPAERO, Université de Toulouse, Toulouse, France
| | | | | | | | | | | | | | - Leslie Tamppari
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
| | | | | | - Maria Genzer
- Finnish Meteorological Institute, Helsinki, Finland
| | - Maria Hieta
- Finnish Meteorological Institute, Helsinki, Finland
| | | | - Pan Conrad
- Carnegie Institution for Science, Washington, DC, USA
| | | | | | - David Mimoun
- ISAE-SUPAERO, Université de Toulouse, Toulouse, France
| | | | | | | | - Justin N. Maki
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
| | | | - Roger C. Wiens
- Los Alamos National Laboratory, Los Alamos, NM, USA
- Purdue University, West Lafayette, IN, USA
| | | | | | | | - Luis Mora
- Centro de Astrobiologia, INTA, Madrid, Spain
| | - Mariah M. Baker
- Smithsonian National Air and Space Museum, Washington, DC, USA
| | - Don Banfield
- Cornell University, Ithaca, NY, USA
- NASA Ames, Mountain View, CA, USA
| | - Jorge Pla-Garcia
- Space Science Institute, Boulder, CO, USA
- Centro de Astrobiologia, INTA, Madrid, Spain
| | | | | | - Ben Clark
- Space Science Institute, Boulder, CO, USA
| | | | | | | | - Priyaben Patel
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
- UCL, London, UK
| | | | | | - Raymond Francis
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
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Piqueux S, Müller N, Grott M, Siegler M, Millour E, Forget F, Lemmon M, Golombek M, Williams N, Grant J, Warner N, Ansan V, Daubar I, Knollenberg J, Maki J, Spiga A, Banfield D, Spohn T, Smrekar S, Banerdt B. Soil Thermophysical Properties Near the InSight Lander Derived From 50 Sols of Radiometer Measurements. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2021; 126:e2021JE006859. [PMID: 35845552 PMCID: PMC9285084 DOI: 10.1029/2021je006859] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/21/2021] [Revised: 04/12/2021] [Accepted: 04/19/2021] [Indexed: 06/11/2023]
Abstract
Measurements from the InSight lander radiometer acquired after landing are used to characterize the thermophysical properties of the Martian soil in Homestead hollow. This data set is unique as it stems from a high measurement cadence fixed platform studying a simple well-characterized surface, and it benefits from the environmental characterization provided by other instruments. We focus on observations acquired before the arrival of a regional dust storm (near Sol 50), on the furthest observed patch of soil (i.e., ∼3.5 m away from the edge of the lander deck) where temperatures are least impacted by the presence of the lander and where the soil has been least disrupted during landing. Diurnal temperature cycles are fit using a homogenous soil configuration with a thermal inertia of 183 ± 25 J m-2 K-1 s-1/2 and an albedo of 0.16, corresponding to very fine to fine sand with the vast majority of particles smaller than 140 μm. A pre-landing assessment leveraging orbital thermal infrared data is consistent with these results, but our analysis of the full diurnal temperature cycle acquired from the ground further indicates that near surface layers with different thermophysical properties must be thin (i.e., typically within the top few mm) and deep layering with different thermophysical properties must be at least below ∼4 cm. The low thermal inertia value indicates limited soil cementation within the upper one or two skin depths (i.e., ∼4-8 cm and more), with cement volumes <<1%, which is challenging to reconcile with visible images of overhangs in pits.
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Affiliation(s)
- Sylvain Piqueux
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Nils Müller
- DLR Institute for Planetary ResearchBerlinGermany
| | | | | | | | | | | | - Matthew Golombek
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Nathan Williams
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - John Grant
- National Air and Space MuseumSmithsonian InstitutionWashingtonDCUSA
| | | | | | | | | | - Justin Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | - Tilman Spohn
- DLR Institute for Planetary ResearchBerlinGermany
- International Space Science Institute ISSIBernSwitzerland
| | - Susan Smrekar
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Bruce Banerdt
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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Golombek M, Williams N, Warner NH, Parker T, Williams MG, Daubar I, Calef F, Grant J, Bailey P, Abarca H, Deen R, Ruoff N, Maki J, McEwen A, Baugh N, Block K, Tamppari L, Call J, Ladewig J, Stoltz A, Weems WA, Mora‐Sotomayor L, Torres J, Johnson M, Kennedy T, Sklyanskiy E. Location and Setting of the Mars InSight Lander, Instruments, and Landing Site. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2020; 7:e2020EA001248. [PMID: 33134434 PMCID: PMC7583488 DOI: 10.1029/2020ea001248] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/29/2020] [Revised: 09/09/2020] [Accepted: 09/12/2020] [Indexed: 06/11/2023]
Abstract
Knowing precisely where a spacecraft lands on Mars is important for understanding the regional and local context, setting, and the offset between the inertial and cartographic frames. For the InSight spacecraft, the payload of geophysical and environmental sensors also particularly benefits from knowing exactly where the instruments are located. A ~30 cm/pixel image acquired from orbit after landing clearly resolves the lander and the large circular solar panels. This image was carefully georeferenced to a hierarchically generated and coregistered set of decreasing resolution orthoimages and digital elevation models to the established positive east, planetocentric coordinate system. The lander is located at 4.502384°N, 135.623447°E at an elevation of -2,613.426 m with respect to the geoid in Elysium Planitia. Instrument locations (and the magnetometer orientation) are derived by transforming from Instrument Deployment Arm, spacecraft mechanical, and site frames into the cartographic frame. A viewshed created from 1.5 m above the lander and the high-resolution orbital digital elevation model shows the lander is on a shallow regional slope down to the east that reveals crater rims on the east horizon ~400 m and 2.4 km away. A slope up to the north limits the horizon to about 50 m away where three rocks and an eolian bedform are visible on the rim of a degraded crater rim. Azimuths to rocks and craters identified in both surface panoramas and high-resolution orbital images reveal that north in the site frame and the cartographic frame are the same (within 1°).
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Affiliation(s)
- M. Golombek
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - N. Williams
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - N. H. Warner
- Department of Geological SciencesSUNY GeneseoGeneseoNYUSA
| | - T. Parker
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - M. G. Williams
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - I. Daubar
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
- Department of Earth, Environmental, and Planetary SciencesBrown UniversityProvidenceRIUSA
| | - F. Calef
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Grant
- Smithsonian Institution, National Air and Space MuseumWashingtonDCUSA
| | - P. Bailey
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - H. Abarca
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - R. Deen
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - N. Ruoff
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - A. McEwen
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - N. Baugh
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - K. Block
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - L. Tamppari
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Call
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | | | - L. Mora‐Sotomayor
- Centro de Astrobiología (CSIC/INTA)Instituto Nacional de Técnica AeroespacialMadridSpain
| | - J. Torres
- Centro de Astrobiología (CSIC/INTA)Instituto Nacional de Técnica AeroespacialMadridSpain
| | | | | | - E. Sklyanskiy
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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