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Distribution and evolution of scalloped terrain in the southern hemisphere, Mars

Zanetti, Michael und Hiesinger, Harald und Reiss, Dennis und Hauber, Ernst und Neukum, Gerhard (2010) Distribution and evolution of scalloped terrain in the southern hemisphere, Mars. Icarus: International Journal of Solar System Studies, 206, Seiten 691-706. Elsevier. doi: 10.1016/j.icarus.2009.09.010.

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Offizielle URL: http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WGF-4XBG1C6-3&_user=100058&_coverDate=04%2F30%2F2010&_rdoc=1&_fmt=high&_orig=search&_origin=search&_sort=d&_docanchor=&view=c&_acct=C000007338&_version=1&_urlVersion=0&_userid=100058&md5=16e0a5053

Kurzfassung

Scalloped depressions are a unique martian surface morphology found in the northern and southern hemisphere latitude-dependent dust and ice-rich surface mantles. These features exhibit a distinct asymmetric north�south slope profile, characterized by steep pole-facing scarps, flat floors and gentle equatorfacing slopes. We examined High Resolution Stereo Camera (HRSC) images of the southern hemisphere to determine their longitudinal distribution, which revealed that a majority of scalloped terrain is located in the region of the southern wall of the Hellas Basin and northern Malea Planum. A detailed map of this area was produced where scallops were found to contour the southern wall of the basin, and where the ice-rich mantle was seen to be thickest. Scalloped terrain is concentrated along the topographic highs near the Amphitrites and Peneus Paterae and areal extent and depth decreases with increasing depth into the basin. We also examined existing hypothesis for the formation and evolution of scalloped depressions using High Resolution Imaging Science Experiment (HiRISE) images and data from the Thermal Emission Imaging System�Infrared (THEMIS�IR) and the Thermal Emission Spectrometer (TES). Our approach provides regional context for the development of scalloped terrains within the southern hemisphere, and offers detailed evidence of scallop depressions forming around small cracks, presumably caused by thermal contraction. Morphometric measurements show that scalloped depressions can be as much as 40 m deep, with typical depths of between 10 and 20 m. Our observations of scallop formation and development in the southern hemisphere support a solar-insolation model proposed by previous researchers (e.g. [Morgenstern, A., Hauber, E., Reiss, D., van Gasselt, S., Grosse, G., Schirrmeister, L., 2007. J. Geophys. Res. 112, CiteID E06010; Lefort, A., Russell, P.S., Thomas, N., McEwen, A.S., Dundas, C.M., Kirk, R.L., 2009a. J. Geophys. Res. 114, E04005; Lefort, A., Russell, P.S., Thomas, N., 2009b. Icarus, in press]). Observations made using HiRISE images suggest that scalloped depressions most likely form from small cracks in the mantle, which become larger and deeper through sublimation of interstitial ice from within the mantle. Sublimation is likely enhanced on equator-facing slopes because of increased solar insolation, which accounts for the asymmetric slope profile and hemispherical orientation and is demonstrated by THEMISIR images. We suggest that sublimation lag deposits can possibly be removed by dust devils or strong slope winds related to the Hellas Basin, offering an explanation as to why scalloped terrain is so abundant only in this area of the southern hemisphere. Daytime maximum summer temperatures suggest that sublimation in the study area of Malea Planum is possible under current conditions if the sublimation lag is removed. While it cannot be ruled out that scalloped terrain in Malea Planum is presently evolving, we attribute the extensive distribution to geologically recent obliquity excursions when conditions were more conducive to mesoscale modification of the ice-rich mantle.

elib-URL des Eintrags:https://elib.dlr.de/67521/
Dokumentart:Zeitschriftenbeitrag
Titel:Distribution and evolution of scalloped terrain in the southern hemisphere, Mars
Autoren:
AutorenInstitution oder E-Mail-AdresseAutoren-ORCID-iDORCID Put Code
Zanetti, MichaelInstitute für Planetologie, Westfälische Wilhelms–Universität MünsterNICHT SPEZIFIZIERTNICHT SPEZIFIZIERT
Hiesinger, HaraldInstitute für Planetologie, Westfälische Wilhelms–Universität MünsterNICHT SPEZIFIZIERTNICHT SPEZIFIZIERT
Reiss, DennisInstitute für Planetologie, Westfälische Wilhelms–Universität MünsterNICHT SPEZIFIZIERTNICHT SPEZIFIZIERT
Hauber, Ernsternst.hauber (at) dlr.deNICHT SPEZIFIZIERTNICHT SPEZIFIZIERT
Neukum, GerhardFU BerlinNICHT SPEZIFIZIERTNICHT SPEZIFIZIERT
Datum:2010
Erschienen in:Icarus: International Journal of Solar System Studies
Referierte Publikation:Ja
Open Access:Nein
Gold Open Access:Nein
In SCOPUS:Ja
In ISI Web of Science:Ja
Band:206
DOI:10.1016/j.icarus.2009.09.010
Seitenbereich:Seiten 691-706
Verlag:Elsevier
Status:veröffentlicht
Stichwörter:Mars, ice, water, thermokarst, permafrost, climate
HGF - Forschungsbereich:Verkehr und Weltraum (alt)
HGF - Programm:Weltraum (alt)
HGF - Programmthema:W EW - Erforschung des Weltraums
DLR - Schwerpunkt:Weltraum
DLR - Forschungsgebiet:W EW - Erforschung des Weltraums
DLR - Teilgebiet (Projekt, Vorhaben):W - Projekt MARS-EXPRESS / HRSC (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Planetengeologie
Hinterlegt von: Hauber, Ernst
Hinterlegt am:06 Jan 2011 13:23
Letzte Änderung:10 Jan 2019 15:47

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