Determination of local surface properties using Mars Express bistatic radar

Simpson, R. A.; Tyler, G. L.; Pätzold, M.; Häusler, B.

doi:10.1029/2005je002580

Cited by 12 publications

(8 citation statements)

References 5 publications

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“…The SHARAD (Shallow Radar) instrument on MRO (Mars Reconnaissance Orbiter) sounded through thin Amazonis Planitia plains materials and the Vastitas Borealis Formation, and the measured loss tangents of 0.005 -0.012 are consistent with moderatedensity sediments [Campbell et al, 2008]. Bistatic experiments between the orbiting Mars Express spacecraft and the NASA Goldstone antennas at a wavelength of 3.6 cm yielded permittivity values between 2 and 4 across a variety of Martian terrains including the poles and northern plains [Simpson et al, 2007]. Using Arecibo Observatory as a receiver at 13 cm wavelength resulted in permittivity estimates that were 10-50% higher than the 3.6 cm wavelength data across the same terrains [Simpson et al, 2007], consistent with an increase in dust compaction or a transition to dense bedrock in the upper 1 m of the Martian surface.…”

Section: Introductionmentioning

confidence: 94%

“…Bistatic experiments between the orbiting Mars Express spacecraft and the NASA Goldstone antennas at a wavelength of 3.6 cm yielded permittivity values between 2 and 4 across a variety of Martian terrains including the poles and northern plains [Simpson et al, 2007]. Using Arecibo Observatory as a receiver at 13 cm wavelength resulted in permittivity estimates that were 10-50% higher than the 3.6 cm wavelength data across the same terrains [Simpson et al, 2007], consistent with an increase in dust compaction or a transition to dense bedrock in the upper 1 m of the Martian surface. If basaltic lava flows cover considerable areas of Mars, one might expect to see higher measured permittivity values.…”

Section: Introductionmentioning

confidence: 99%

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Dielectric properties of lava flows west of Ascraeus Mons, Mars

Carter

Campbell

Holt

et al. 2009

Geophysical Research Letters

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The SHARAD instrument on the Mars Reconnaissance Orbiter detects subsurface interfaces beneath lava flow fields northwest of Ascraeus Mons. The interfaces occur in two locations; a northern flow that originates south of Alba Patera, and a southern flow that originates at the rift zone between Ascraeus and Pavonis Montes. The northern flow has permittivity values, estimated from the time delay of echoes from the basal interface, between 6.2 and 17.3, with an average of 12.2. The southern flow has permittivity values of 7.0 to 14.0, with an average of 9.8. The average permittivity values for the northern and southern flows imply densities of 3.7 and 3.4 g cm−3, respectively. Loss tangent values for both flows range from 0.01 to 0.03. The measured bulk permittivity and loss tangent values are consistent with those of terrestrial and lunar basalts, and represent the first measurement of these properties for dense rock on Mars.

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Section: Introductionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Dielectric properties of lava flows west of Ascraeus Mons, Mars

Carter

Campbell

Holt

et al. 2009

Geophysical Research Letters

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“…Regions A and D were predicted to have the thinnest soil cover, region C an intermediate value, and region B the thickest cover. Detailed examination of MOC images, thermal inertia values derived from TES data [ Putzig and Mellon , 2007], and Earth‐based radar cross sections [ Simpson et al , 2006] suggested soil exposures dominated all regions. Attempts were made to determine the areal fraction of the surface occupied by rocks by modeling the surface as soil and rock covers and examining the nonisothermal properties in emission due to this two component mixture [e.g., Christensen , 1986].…”

Section: Search For Safe Landing Sitesmentioning

confidence: 99%

Mars Exploration Program 2007 Phoenix landing site selection and characteristics

Arvidson¹,

Adams

Bonfiglio

et al. 2008

J. Geophys. Res.

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[1] To ensure a successful touchdown and subsequent surface operations, the Mars Exploration Program 2007 Phoenix Lander must land within 65°to 72°north latitude, at an elevation less than À3.5 km. The landing site must have relatively low wind velocities and rock and slope distributions similar to or more benign than those found at the Viking Lander 2 site. Also, the site must have a soil cover of at least several centimeters over ice or icy soil to meet science objectives of evaluating the environmental and habitability implications of past and current near-polar environments. The most challenging aspects of site selection were the extensive rock fields associated with crater rims and ejecta deposits and the centers of polygons associated with patterned ground. An extensive acquisition campaign of Odyssey Thermal Emission Imaging Spectrometer predawn thermal IR images, together with $0.31 m/pixel Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment images was implemented to find regions with acceptable rock populations and to support Monte Carlo landing simulations. The chosen site is located at 68.16°north latitude, 233.35°east longitude (areocentric), within a $50 km wide (N-S) by $300 km long (E-W) valley of relatively rock-free plains. Surfaces within the eastern portion of the valley are differentially eroded ejecta deposits from the relatively recent $10-km-wide Heimdall crater and have fewer rocks than plains on the western portion of the valley. All surfaces exhibit polygonal ground, which is associated with fracture of icy soils, and are predicted to have only several centimeters of poorly sorted basaltic sand and dust over icy soil deposits.

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“…According to Ref. [26], the dielectric constant is in the range of 2∼4, while higher values of dielectric constants at northern hemisphere were reported [6]. In this paper, we set the dielectric constant to 3.…”

Section: Numerical Results and Analysismentioning

confidence: 99%

L‐band depolarised radar back scattering from Martian topographic surface: A numerical study

Yang

Liu

Chen

et al. 2021

IET Radar Sonar & Navi

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The interaction of radar signals with a planetary surface is critical for the utility of radar data. Herein, a power-law roughness spectrum is used to model the roughness and an inhomogeneous vertical permittivity to describe the dielectrics from the surface of Mars. Numerical simulations of depolarised radar backscattering are then conducted. To gain a more complete picture of depolarised characteristics, a wide range of surface roughness is considered. Results reveal that the depolarised backscattering is sensitive to the dielectric profiles with-10 dB is observed. The polarization conversion ratio, the ratio of depolarisation to total polarization backscattering, is a sensitive indicator of dielectric profiles and roughness, and thus is useful in retrieving dielectric profile. This is an open access article under the terms of the Creative Commons Attribution-NonCommercial-NoDerivs License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non-commercial and no modifications or adaptations are made.

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Determination of local surface properties using Mars Express bistatic radar

Cited by 12 publications

References 5 publications

Dielectric properties of lava flows west of Ascraeus Mons, Mars

Dielectric properties of lava flows west of Ascraeus Mons, Mars

Mars Exploration Program 2007 Phoenix landing site selection and characteristics

L‐band depolarised radar back scattering from Martian topographic surface: A numerical study

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