1
|
A Concept for a Mars Boundary Layer Sounding Balloon: Science Case, Technical Concept and Deployment Risk Analysis. AEROSPACE 2022. [DOI: 10.3390/aerospace9030136] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
The Mars Exploration Program Analysis Group has identified measurements of the state and the variability of the Martian atmosphere as high priority investigations for the upcoming years. Balloon-borne instruments could bridge the gap in both temporal and spatial resolution in mesoscale distances between local, stationary landers and global orbiter observations. The idea to use a balloon system for such a purpose is not new in essence and has been proposed already in past decades. While those concepts considered an aerial deployment during entry and descent, the concept outlined in this study revisits a launch off the payload deck of a lander from the Martian surface. This deployment option profits today mainly from the technological advance in micro-electronics and sensor miniaturization, which enables the design of a balloon-probe significantly smaller than earlier proposed systems. This paper presents the feasibility assessment for this instrument and gives further details on the scientific and operational concept, a strawman sensor suite, its system components and the associated size and budget estimates. It is complemented by the analysis scheme proposed to assess, manage and mitigate the deployment risk involved in automatically launching such a balloon-system off a planetary surface.
Collapse
|
2
|
Clancy RT, Wolff MJ, Heavens NG, James PB, Lee SW, Sandor BJ, Cantor BA, Malin MC, Tyler D, Spiga A. Mars Perihelion Cloud Trails as revealed by MARCI: Mesoscale Topographically Focussed Updrafts and Gravity Wave Forcing of High Altitude Clouds. ICARUS 2021; 362:114411. [PMID: 33867569 PMCID: PMC8051166 DOI: 10.1016/j.icarus.2021.114411] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Daily, global wide angle imaging of Mars clouds in MARCI (MARs Color Imager, (Malin et al., 2008)) ultraviolet and visible bands reveals the spatial/seasonal distributions and physical characteristics of perihelion cloud trails (PCT); a class of high altitude (40-50 km), horizontally extended (200-1000 km, trending W to WSW) water ice clouds formed over specific southern low-to-mid latitude (5S-40S), mesoscale (~50 km) locations during the Mars perihelion, southern summer season. PCT were first reported in association with rim regions of Valles Marineris (Clancy et al., 2009). The current study employs MARCI 2007-2011 imaging to sample the broader distributions and properties of PCT; and indicates several distinct locations of peak occurrences, including SW Arsia Mons, elevated regions of Syria, Solis, and Thaumasia Planitia, along Valles Marineris margins, and the NE rim of Hellas Basin. PCT are present over Mars solar longitudes (L S ) of 210-310°, in late morning to mid afternoon hours (10am-3pm), and are among the brightest and most distinctive clouds exhibited during the perihelion portion of the Mars orbit. Their locations (i.e., eastern margin origins) correspond to strong local elevation gradients, and their timing to peak solar heating conditions (perihelion, subsolar latitudes and midday local times). They occur approximately on a daily basis among all locations identified (i.e., not daily at a single location). Based on cloud surface shadow analyses, PCT form at 40-50 km aeroid altitudes, where water vapor is generally at near-saturation conditions in this perihelion period (e.g. Millour et al., 2014). They exhibited notable absences during periods of planet encircling and regional dust storm activity in 2007 and 2009, respectively, presumably due to reduced water saturation conditions above 35-40 km altitudes associated with increased dust heating over the vertically extended atmosphere (e.g., Neary et al., 2019). PCT exhibit smaller particle sizes (R eff =0.2-0.5μm) than typically exhibited in the lower atmosphere, and incorporate significant fractions of available water vapor at these altitudes. PCT ice particles are inferred to form continuously (over ~4 hours) at their PCT eastern origins, associated with localized updrafts, and are entrained in upper level zonal/meridional winds (towards W or WSW with ~50 m/sec speeds at 40-50 km altitudes) to create long, linear cloud trails. PCT cloud formation is apparently forced in the lower atmosphere (≤10-15 km) by strong updrafts associated with distinctive topographic gradients, such as simulated in mesoscale studies (e.g., Tyler and Barnes, 2015) and indicated by the surface-specific PCT locations. These lower scale height updrafts are proposed to generate vertically propagating gravity waves (GW), leading to PCT formation above ~40 km altitudes where water vapor saturation conditions promote vigorous cloud ice formation. Recent mapping of GW amplitudes at ~25 km altitudes, from Mars Climate Sounder 15 μm radiance variations (Heavens et al., 2020), in fact demonstrates close correspondences to the detailed spatial distributions of observed PCT, relative to other potential factors such as surface albedo and surface elevation (or related boundary layer depths).
Collapse
Affiliation(s)
- R Todd Clancy
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - Michael J Wolff
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - Nicholas G Heavens
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - Philip B James
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - Steven W Lee
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - Brad J Sandor
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - Bruce A Cantor
- Malin Space Science Systems, 5880 Pacific Center Blvd, San Diego, CA 92121, USA
| | - Michael C Malin
- Malin Space Science Systems, 5880 Pacific Center Blvd, San Diego, CA 92121, USA
| | - Daniel Tyler
- College of Earth Oceanic and Atmospheric Science, Oregon State University, Corvallis, OR 97331, USA
| | - Aymeric Spiga
- Laboratoire de Météorologie Dynamique/Institut Pierre-Simon Laplace (LMD/IPSL), Sorbonne Universités, UPMC Univ Paris 06, PSL Research University, France
| |
Collapse
|
3
|
Abstract
Recurring Slope Lineae (RSL) on Mars have been enigmatic since their discovery; their behavior resembles a seeping liquid but sources of water remain puzzling. This work demonstrates that the properties of RSL are consistent with observed behaviors of Martian and terrestrial aeolian processes. Specifically, RSL are well-explained as flows of sand that remove a thin coating of dust. Observed RSL properties are supportive of or consistent with this model, which requires no liquid water or other exotic processes, but rather indicates seasonal aeolian behavior. These settings and behaviors resemble features observed by rovers and also explain the occurrence of many slope lineae on Mars that do not meet the strict definition of RSL. This indicates that RSL can be explained simply as aeolian features. Other processes may add complexities just as they could modify the behavior of any sand dune.
Collapse
Affiliation(s)
- Colin M. Dundas
- U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA
| |
Collapse
|
4
|
Breuer H, Berényi A, Mari L, Nagy B, Szalai Z, Tordai Á, Weidinger T. Analog Site Experiment in the High Andes-Atacama Region: Surface Energy Budget Components on Ojos del Salado from Field Measurements and WRF Simulations. ASTROBIOLOGY 2020; 20:684-700. [PMID: 32048870 DOI: 10.1089/ast.2019.2024] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Remote sensing data are abundant, whereas surface in situ verification of atmospheric conditions is rare on Mars. Earth-based analogs could help gain an understanding of soil and atmospheric processes on Mars and refine existing models. In this work, we evaluate the applicability of the Weather Research and Forecasting (WRF) model against measurements from the Mars analog High Andes-Atacama Desert. Validation focuses on the surface conditions and on the surface energy budget. Measurements show that the average daily net radiation, global radiation, and latent heat flux amount to 131, 273, and about 10 W/m2, respectively, indicating extremely dry atmospheric conditions. Dynamically, the effect of topography is also well simulated. One of the main modeling problems is the inaccurate initial soil and surface conditions in the area. Correction of soil moisture based on in situ and satellite soil moisture measurements, as well as the removal of snow coverage, reduced the surface skin temperature root mean square error from 9.8°C to 4.3°C. The model, however, has shortcomings when soil condition modeling is considered. Sensible heat flux estimations are on par with the measurements (daily maxima around 500 W/m2), but surface soil heat flux is greatly overestimated (by 150-500 W/m2). Soil temperature and soil moisture diurnal variations are inconsistent with the measurements, partially due to the lack of water vapor representation in soil calculations.
Collapse
Affiliation(s)
- Hajnalka Breuer
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| | - Alexandra Berényi
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| | - László Mari
- Department of Physical Geography, Eötvös Loránd University, Budapest, Hungary
| | - Balázs Nagy
- Department of Physical Geography, Eötvös Loránd University, Budapest, Hungary
| | - Zoltán Szalai
- Department of Environmental and Landscape Geography, Eötvös Loránd University, Budapest, Hungary
- Geographical Research Institute, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Budapest, Hungary
| | - Ágoston Tordai
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| | - Tamás Weidinger
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| |
Collapse
|
5
|
Heavens NG, Kass DM, Shirley JH. Dusty Deep Convection in the Mars Year 34 Planet-Encircling Dust Event. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2019; 124:2863-2892. [PMID: 32908808 PMCID: PMC7477802 DOI: 10.1029/2019je006110] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/03/2019] [Accepted: 09/19/2019] [Indexed: 06/11/2023]
Abstract
Dusty convection, convective activity powered by radiative heating of dust, is a ubiquitous phenomenon in Mars's atmosphere but is especially deep (that is, impactful on the middle atmosphere) and widespread during planet-encircling dust events (PEDE) that occur every few Mars Years (MY). Yet the relative roles of dusty deep convection and global dynamics, such as the principal meridional overturning cell (PMOC) and the radiative tides, in dust storm development and the vertical transport of dust and water are still unclear. Here, observations from the Mars Climate Sounder on board Mars Reconnaissance Orbiter (MRO-MCS) are used to study dusty deep convection and its impact on middle atmospheric water content during the MY 34 PEDE (commenced June 2018). Additional context is provided by MRO-MCS observations of the MY 28 PEDE (commenced June 2007). This investigation establishes that a few, localized centers of dusty deep convection in the tropics formed in the initial phases of both PEDE simultaneously with a substantial increase in middle atmospheric water content. The growth phase of the MY 34 PEDE was defined by episodic outbreaks of deep convection along the Acidalia and Utopia storm tracks as opposed to less episodic, more longitudinally distributed convective activity during the MY 28 PEDE. The most intense convection during both PEDE was observed in southern/eastern Tharsis, where MRO-MCS observed multiple instances of deep convective clouds transporting dust to altitudes of 70-90 km. These results suggest that Martian PEDE typically contain multiple convectively active mesoscale weather systems.
Collapse
Affiliation(s)
- Nicholas G. Heavens
- Department of Atmospheric and Planetary Sciences, Hampton University, 154 William R. Harvey Way, Hampton, Virginia, 23668, USA
- Space Science Institute, 4750 Walnut St., # 205, Boulder, Colorado, 80301, USA
| | - David M. Kass
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
| | - James H. Shirley
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
| |
Collapse
|
6
|
The dune effect on sand-transporting winds on Mars. Nat Commun 2015; 6:8796. [PMID: 26537669 PMCID: PMC4667610 DOI: 10.1038/ncomms9796] [Citation(s) in RCA: 35] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/01/2015] [Accepted: 10/06/2015] [Indexed: 11/15/2022] Open
Abstract
Wind on Mars is a significant agent of contemporary surface change, yet the absence of in situ meteorological data hampers the understanding of surface–atmospheric interactions. Airflow models at length scales relevant to landform size now enable examination of conditions that might activate even small-scale bedforms (ripples) under certain contemporary wind regimes. Ripples have the potential to be used as modern ‘wind vanes' on Mars. Here we use 3D airflow modelling to demonstrate that local dune topography exerts a strong influence on wind speed and direction and that ripple movement likely reflects steered wind direction for certain dune ridge shapes. The poor correlation of dune orientation with effective sand-transporting winds suggests that large dunes may not be mobile under modelled wind scenarios. This work highlights the need to first model winds at high resolution before inferring regional wind patterns from ripple movement or dune orientations on the surface of Mars today. The absence of in situ and long-term meteorological data hampers our understanding of wind movement on Mars. Here, the authors use 3D airflow modelling to investigate small scale ripple migration and suggest that local dune topography exerts a strong influence on wind speed and direction.
Collapse
|
7
|
Kok JF, Parteli EJR, Michaels TI, Karam DB. The physics of wind-blown sand and dust. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2012; 75:106901. [PMID: 22982806 DOI: 10.1088/0034-4885/75/10/106901] [Citation(s) in RCA: 160] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/12/2023]
Abstract
The transport of sand and dust by wind is a potent erosional force, creates sand dunes and ripples, and loads the atmosphere with suspended dust aerosols. This paper presents an extensive review of the physics of wind-blown sand and dust on Earth and Mars. Specifically, we review the physics of aeolian saltation, the formation and development of sand dunes and ripples, the physics of dust aerosol emission, the weather phenomena that trigger dust storms, and the lifting of dust by dust devils and other small-scale vortices. We also discuss the physics of wind-blown sand and dune formation on Venus and Titan.
Collapse
Affiliation(s)
- Jasper F Kok
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY, USA.
| | | | | | | |
Collapse
|
8
|
Chojnacki M, Burr DM, Moersch JE, Michaels TI. Orbital observations of contemporary dune activity in Endeavor crater, Meridiani Planum, Mars. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003675] [Citation(s) in RCA: 78] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
9
|
Hayward RK, Titus TN, Michaels TI, Fenton LK, Colaprete A, Christensen PR. Aeolian dunes as ground truth for atmospheric modeling on Mars. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003428] [Citation(s) in RCA: 41] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
10
|
Spiga A, Forget F. A new model to simulate the Martian mesoscale and microscale atmospheric circulation: Validation and first results. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003242] [Citation(s) in RCA: 98] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
11
|
Chojnacki M, Hynek BM. Geological context of water-altered minerals in Valles Marineris, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003070] [Citation(s) in RCA: 43] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
12
|
Tamppari LK, Barnes J, Bonfiglio E, Cantor B, Friedson AJ, Ghosh A, Grover MR, Kass D, Martin TZ, Mellon M, Michaels T, Murphy J, Rafkin SCR, Smith MD, Tsuyuki G, Tyler D, Wolff M. Expected atmospheric environment for the Phoenix landing season and location. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003034] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
13
|
Kauhanen J, Siili T, Järvenoja S, Savijärvi H. The Mars limited area model and simulations of atmospheric circulations for the Phoenix landing area and season of operation. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003011] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
14
|
Michaels TI, Rafkin SCR. Meteorological predictions for candidate 2007 Phoenix Mars Lander sites using the Mars Regional Atmospheric Modeling System (MRAMS). ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003013] [Citation(s) in RCA: 27] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
15
|
Sullivan R, Arvidson R, Bell JF, Gellert R, Golombek M, Greeley R, Herkenhoff K, Johnson J, Thompson S, Whelley P, Wray J. Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at “El Dorado” and surroundings at Gusev Crater. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003101] [Citation(s) in RCA: 220] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
16
|
Greeley R, Whelley PL, Neakrase LDV, Arvidson RE, Bridges NT, Cabrol NA, Christensen PR, Di K, Foley DJ, Golombek MP, Herkenhoff K, Knudson A, Kuzmin RO, Li R, Michaels T, Squyres SW, Sullivan R, Thompson SD. Columbia Hills, Mars: Aeolian features seen from the ground and orbit. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002971] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
17
|
Spiga A, Forget F, Dolla B, Vinatier S, Melchiorri R, Drossart P, Gendrin A, Bibring JP, Langevin Y, Gondet B. Remote sensing of surface pressure on Mars with the Mars Express/OMEGA spectrometer: 2. Meteorological maps. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002870] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Aymeric Spiga
- Laboratoire de Météorologie Dynamique; Institut Pierre-Simon Laplace; Paris France
| | - François Forget
- Laboratoire de Météorologie Dynamique; Institut Pierre-Simon Laplace; Paris France
| | - Bastien Dolla
- Laboratoire de Météorologie Dynamique; Institut Pierre-Simon Laplace; Paris France
| | | | | | | | | | | | | | | |
Collapse
|
18
|
Greeley R, Whelley PL, Arvidson RE, Cabrol NA, Foley DJ, Franklin BJ, Geissler PG, Golombek MP, Kuzmin RO, Landis GA, Lemmon MT, Neakrase LDV, Squyres SW, Thompson SD. Active dust devils in Gusev crater, Mars: Observations from the Mars Exploration Rover Spirit. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002743] [Citation(s) in RCA: 114] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ronald Greeley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | - Patrick L. Whelley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University in St. Louis; St. Louis Missouri USA
| | | | - Daniel J. Foley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | | | - Paul G. Geissler
- Astrogeology Program; U.S. Geological Survey; Flagstaff Arizona USA
| | | | | | | | - Mark T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - Lynn D. V. Neakrase
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | | | - Shane D. Thompson
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| |
Collapse
|
19
|
Greeley R, Arvidson RE, Barlett PW, Blaney D, Cabrol NA, Christensen PR, Fergason RL, Golombek MP, Landis GA, Lemmon MT, McLennan SM, Maki JN, Michaels T, Moersch JE, Neakrase LDV, Rafkin SCR, Richter L, Squyres SW, de Souza PA, Sullivan RJ, Thompson SD, Whelley PL. Gusev crater: Wind-related features and processes observed by the Mars Exploration Rover Spirit. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002491] [Citation(s) in RCA: 125] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ronald Greeley
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - R. E. Arvidson
- Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | - Diana Blaney
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - N. A. Cabrol
- NASA Ames Research Center; Moffett Field California USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - R. L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - M. P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - M. T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - S. M. McLennan
- Department of Geosciences; State University of New York at Stony Brook; Stony Brook New York USA
| | - J. N. Maki
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - J. E. Moersch
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - L. D. V. Neakrase
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - Lutz Richter
- Institut für Raumsimulation; Deutschen Zentrum für Luft- und Raumfahrt; Cologne Germany
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| | | | - R. J. Sullivan
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. D. Thompson
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - P. L. Whelley
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| |
Collapse
|
20
|
Greeley R. Martian variable features: New insight from the Mars Express Orbiter and the Mars Exploration Rover Spirit. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002403] [Citation(s) in RCA: 61] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
21
|
|
22
|
Kirk RL, Howington-Kraus E, Redding B, Galuszka D, Hare TM, Archinal BA, Soderblom LA, Barrett JM. High-resolution topomapping of candidate MER landing sites with Mars Orbiter Camera narrow-angle images. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002131] [Citation(s) in RCA: 97] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Randolph L. Kirk
- Astrogeology Team; U.S. Geological Survey; Flagstaff Arizona USA
| | | | - Bonnie Redding
- Astrogeology Team; U.S. Geological Survey; Flagstaff Arizona USA
| | - Donna Galuszka
- Astrogeology Team; U.S. Geological Survey; Flagstaff Arizona USA
| | - Trent M. Hare
- Astrogeology Team; U.S. Geological Survey; Flagstaff Arizona USA
| | | | | | - Janet M. Barrett
- Astrogeology Team; U.S. Geological Survey; Flagstaff Arizona USA
| |
Collapse
|
23
|
Golombek MP, Grant JA, Parker TJ, Kass DM, Crisp JA, Squyres SW, Haldemann AFC, Adler M, Lee WJ, Bridges NT, Arvidson RE, Carr MH, Kirk RL, Knocke PC, Roncoli RB, Weitz CM, Schofield JT, Zurek RW, Christensen PR, Fergason RL, Anderson FS, Rice JW. Selection of the Mars Exploration Rover landing sites. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002074] [Citation(s) in RCA: 126] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- M. P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. A. Grant
- Center for Earth and Planetary Studies; National Air and Space Museum, Smithsonian Institution; Washington DC USA
| | - T. J. Parker
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - D. M. Kass
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. A. Crisp
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - A. F. C. Haldemann
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - M. Adler
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - W. J. Lee
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - N. T. Bridges
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. E. Arvidson
- Department of Earth and Space Sciences; Washington University; St. Louis Missouri USA
| | - M. H. Carr
- U.S. Geological Survey; Menlo Park California USA
| | - R. L. Kirk
- U.S. Geological Survey; Flagstaff Arizona USA
| | - P. C. Knocke
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. B. Roncoli
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - J. T. Schofield
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. W. Zurek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - R. L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - F. S. Anderson
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. W. Rice
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| |
Collapse
|
24
|
Kass DM, Schofield JT, Michaels TI, Rafkin SCR, Richardson MI, Toigo AD. Analysis of atmospheric mesoscale models for entry, descent, and landing. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002065] [Citation(s) in RCA: 35] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- D. M. Kass
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. T. Schofield
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - T. I. Michaels
- Department of Meteorology; San Jose State University; San Jose California USA
| | - S. C. R. Rafkin
- Department of Meteorology; San Jose State University; San Jose California USA
| | - M. I. Richardson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - A. D. Toigo
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| |
Collapse
|
25
|
Greeley R, Kuzmin RO, Rafkin SCR, Michaels TI, Haberle R. Wind-related features in Gusev crater, Mars. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je002006] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ronald Greeley
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - Scot C. R. Rafkin
- Department of Meteorology; San Jose State University; San Jose California USA
| | - Timothy I. Michaels
- Department of Meteorology; San Jose State University; San Jose California USA
| | | |
Collapse
|