Arecibo radar imagery of Mars: The major volcanic provinces

Harmon, J. K.; Nolan, M. C.; Husmann, Diana I.; Campbell, B. A.

doi:10.1016/j.icarus.2012.06.030

Cited by 56 publications

(31 citation statements)

References 122 publications

(344 reference statements)

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“…We use 12.6-cm radar imaging and polarimetric information obtained by Arecibo Observatory on October 3, 2005 (Harmon et al 2012) to evaluate surface roughness and rock abundance at scales comparable to the radar wavelength. We compare results from the samesense circular (SC) polarization image to that of past landing sites.…”

Section: Arecibo Roughness Analysismentioning

confidence: 99%

Selection of the InSight Landing Site

et al. 2016

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The selection of the Discovery Program InSight landing site took over four years from initial identification of possible areas that met engineering constraints, to downselection via targeted data from orbiters (especially Mars Reconnaissance SPAC 11214 layout: Small Condensed v.2.1 file: spac321.tex (ELE) class: spr-small-v1.2 v.2016/06/09 Prn:2016/12/02; 14:37 p. 1/91» « d o c to p i c : R e v i e w P a p e rn u m b e r i n g s t y l e : C o n t e n t O n l yr e f e r e n c e s t y l e : a p s » latitude (initially 15°S-5°N and later 3°N-5°N for solar power and thermal management of the spacecraft), ellipse size (130 km by 27 km from ballistic entry and descent), and a load bearing surface without thick deposits of dust, severely limited acceptable areas to western Elysium Planitia. Within this area, 16 prospective ellipses were identified, which lie ∼600 km north of the Mars Science Laboratory (MSL) rover. Mapping of terrains in rapidly acquired CTX images identified especially benign smooth terrain and led to the downselection to four northern ellipses. Acquisition of nearly continuous HiRISE, additional Thermal Emission Imaging System (THEMIS), and High Resolution Stereo Camera (HRSC) images, along with radar data confirmed that ellipse E9 met all landing site constraints: with slopes <15°at 84 m and 2 m length scales for radar tracking and touchdown stability, low rock abundance (<10 %) to avoid impact and spacecraft tip over, instrument deployment constraints, which included identical slope and rock abundance constraints, a radar reflective and load bearing surface, and a fragmented regolith ∼5 m thick for full penetration of the heat flow probe. Unlike other Mars landers, science objectives did not directly influence landing site selection. AUTHOR'S PROOF

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Section: Arecibo Roughness Analysismentioning

confidence: 99%

Selection of the InSight Landing Site

et al. 2016

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“…This suggests that the melts are 'rougher' at the centimeter to decimeter scale than most types of terrestrial lavas, which have average CPRs of 0.2 (pahoehoe), 0.5 (a 0 a), and 0.8-1.0 (blocky lavas) at similar incidence angles to Mini-RF (Campbell, 2002). It is notable that lavas on Mars (Harmon et al, 2012) and some impact melts on Mercury (Neish et al, 2013) also have high CPR. The cause of this increased CPR is unknown, but could be the result of either surface or subsurface scattering.…”

Section: Physical Properties Of Impact Melt Depositsmentioning

confidence: 99%

Global distribution of lunar impact melt flows

Neish

Madden

Carter

et al. 2014

Icarus

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“…These models also suggest that Tharsis area lavas, including flows in close proximity to Ascraeus and Pavonis Montes, had viscosities consistent with basaltic composition [ Glaze et al ., ; Baloga and Glaze , ; Glaze and Baloga , ]. Imaging radar data at 12.6 cm wavelength show extensive, radar‐bright flows emanating from the Tharsis Montes [ Harmon et al ., ]. Circular polarization ratios of the radar‐bright flows approach unity, suggesting that the surfaces are rough at the centimeter scale to meter scale and that conditions necessary to produce blocky flow surfaces were common on Mars [ Harmon et al ., ].…”

Section: Introductionmentioning

confidence: 99%

“…Imaging radar data at 12.6 cm wavelength show extensive, radar‐bright flows emanating from the Tharsis Montes [ Harmon et al ., ]. Circular polarization ratios of the radar‐bright flows approach unity, suggesting that the surfaces are rough at the centimeter scale to meter scale and that conditions necessary to produce blocky flow surfaces were common on Mars [ Harmon et al ., ].…”

Section: Introductionmentioning

confidence: 99%

Studies of lava flows in the Tharsis region of Mars using SHARAD

et al. 2014

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The Tharsis region of Mars is covered in volcanic flows that can stretch for tens to hundreds of kilometers. Radar measurements of the dielectric properties of these flows can provide information regarding their composition and density. SHARAD (shallow radar), a sounding radar on the Mars Reconnaissance Orbiter, detects basal interfaces beneath flows in some areas of Tharsis northwest and west of Ascraeus Mons, with additional detections south of Pavonis Mons. Comparisons with 12.6 cm ground-based radar images suggest that SHARAD detects basal interfaces primarily in dust or regolith-mantled regions. We use SHARAD data to estimate the real relative permittivity of the flows by comparing the measured time delay of returns from the subsurface with altimetry measurements of the flow heights relative to the surrounding plains. In cases where the subsurface interface is visible at different depths, spanning tens of meters, it is also possible to measure the loss tangent (tan δ) of the material. The permittivity values calculated range from 7.6 to 11.6, with an average of 9.6, while the mean loss tangent values range from 7.8 × 10À3 to 2.9 × 10 À2with an average of 1.0 × 10 À2. These permittivity and loss tangent estimates for the flows northwest of Ascraeus Mons, west of Ascraeus Mons, and south of Pavonis Mons are consistent with the lab-measured values for dense, low-titanium basalt.

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Arecibo radar imagery of Mars: The major volcanic provinces

Cited by 56 publications

References 122 publications

Selection of the InSight Landing Site

Selection of the InSight Landing Site

Global distribution of lunar impact melt flows

Studies of lava flows in the Tharsis region of Mars using SHARAD

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