As a result of weathering and aeolian processes a fine-grained dark material is distributed all over the Martian surface. On crater floors it is frequently accumulated as dunes. Mobile dunes are probably built and shifted by the actual wind fields. If the dune orientation does not coincide with the actual wind fields, the dunes are assumed fossil. We present a comparison between the actual wind fields and the main orientation of the dune formation. The latter was derived from the dune morphology and wind streaks. The aim of this study is to discriminate between recent and fossil forms of dark material dunes.

For the analysis, we have selected about 50 craters with occurrences of aeolian dark dunes. The data base for the craters is HRSC-Data, which provides a high spectral diversity. High resolution MOC-images are used to analyze the dune shapes. For the actual wind directions modeled wind fields from the Mars Climate Database (MCD) and wind direction data from the Mars Global Reference Atmospheric Model (MarsGRAM Ver. 2001) are used. The results of both datasets will be compared. Additionally, THEMIS nighttime infrared data are used to get information about the brightness temperature of the dune surface, which closely relates to thermal inertia.

Some of the dune fields show a good correlation with the actual wind fields indicating that they might still be active. But others show different wind directions, suggesting fossil forms. This selective mobility and the analysis of the THEMIS-data indicate differences in the surface properties, e.g. consolidation of some dune surfaces

Forget, Francois

Jaumann, Ralf

Jörn, Helbert

Neukum, Gerhard

Poulet, Francois

Reiss, Dennis

Tirsch, Daniela

English

Institute of Transport Research:Publications

INTRODUCTIONWIND DIRECTION DATA FROM THEMARS CLIMATE DATABASE (MCD)BRIGHTNESS TEMPERATURESFROM THEMIS DATACONCLUSIONS FURTHER WORKANALYSIS AND RESULTScorrelative wind directions - cold surface: mobile dune? divergent wind directions - warm surface: fossil dunes?MORPHOLOGY-RELATEDWIND DIRECTIONAs a result of weathering and aeolian processes a fine-graineddark material is distributed all over the Martian surface. Oncrater floors it is frequently accumulated as dunes. Regional-scale controls cause a different morphology and particle sizeof the intracrater materials [1]. The aim of this study is toanalyse the mobility activity of the aeolian material.We have made a comparison between the actual wind fieldsand the main orientation of the dune formation. More over,the surface brightness temperatures were calculated to drawconclusions from the thermal conducivity of the dune surfaces.For this analysis we have selected 50 craters with occurrencesof aeolian dark dunes (Fig. 1). The database for the cratersis HRSC-Data. High resolution MOC-images were used toanalyse the dune shapes. For the actual wind directionsmodelled wind fields from the Mars Climate Database (MCD)are used. THEMIS night-time infrared data were used to getinformation about the brightness temperatures of the dunesurfaces.The MCD is a database of statistics which describes the climate and surfaceenvironment of Mars. It uses two improved state-of-art general circulation models(GCMs) which are based on physical laws and prescribed parameters [2, 3].These models were developed jointly at Laboratoire de Météorologie Dynamiquedu Centre National de la Recherche Scientifique, France, and the Universityof Oxford, United Kingdom, with support of the European Space Agency.For additional information concerning the theoretical background of the GCMssee [2] and [3].THEMIS night-time infrared data were used to derive the brightnesstemperatures (BTR) of the surface materials. The night-time surfacetemperature is closely related to the thermal conductivity of the materialsand thus to the physical structure of the investigated object [5].Fig. 5 shows a THEMIS mosaic of a crater at 15.8°N, 181.5°E withgrey values. Fig. 6 shows a mosaic of the same crater where the greyvalues were conver ted in to  br ightness temperatures.Single THEMIS-BTR images show the absolute brightness temperatureof the surface at the individual solar longitudes of the THEMIS scenes.Note that these THEMIS-BRT mosaics show normalised temperatures.Mobile dunes are built and shifted by the actual wind fields. Ifthe dune orientation does not coincide with the actual windfields the dunes can be assumed to be fossil.The loose (unconsolidated) fine-grained material which coversmobile dune surfaces cools at night more rapidly than coarse-grained sediments and solid rock [6]. If the dune surfaces havewarmer brightness temperatures at night it can be supposedthat the surface could be consolidated.In the following Fig. 7 - 12 the maximum yearly wind directionsfrom the MCD are marked as blue arrows and the wind directionsderived from the dune morphology are marked as red arrows.Fig. 7, 8 and 9 show dune fields with correlativemorphology-related and actual wind directions.The BTRs of this dunes are apparent coolerthan the BTRs of the surrounding indicating thatthey can consist of loos material.The BTRs of the dark materials in  Fig. 10b, 11band 12b show that the dune formations arewarmer at night than the surrounding. Thus itcan be assumed that the dune surfaces couldbe consolidated. The divergent directions of theactual blowing and the morphology-related wind(Fig. 10a, 11a and 12a) confirm this assumption.We wanted to exclude the possibility that theconsolidation could be due to a CO2 frost layer.Therefor the absolute brightness temperaturesof the dune surface were measured at winter-time THEMIS data. For all craters themeasurments show values between 164 K and199 K. These temperatures are to warm for CO2frost [7].40.8 % of the analysed dune fields show a good correlation with the actual wind fields and low night-timesurface temperatures indicating that they might still be active.26.5 % show divergent wind directions, suggesting fossil forms. The warmer BRTs of these dunes indicatethat the surface of these dunes does not consist of fine-grained loose material but could be consolidated.This selective mobility and the analysis of the THEMIS-BTR data indicate fundamental differences in thephysical surface properties of dark material dunes.The measurement of the BTRs of the dune surfaces could exclude that the consolidation of the dune surfacescould be due to CO2 frost.The data used for this analysis [Fig. 2] are yearly  mean and maximum winddirections and wind amplitudes from 10 m above the surface of Mars. Additionally"daily" quantities were took into consideration to get information about the windconditions prevailing at the acquisition date (solar longitude) of the HRSC data.Results of the dune mobility analysis2013680510152025number of cratersfossil dunesno distinct THEMIS informationlocal wind direction not evolvablemobil dunesThe dune morphology, more precisely the slip face orientation,clearly shows the direction of the wind that had built up thedunes. Most of the present dunes shapes are barchan dunes.These dune types have crescentic slip faces that are orientateddownwind [4]. Transverse dunes are also often present. Theyhave downwind orientated slip faces as well. In Fig. 3 thismorphology-related wind direction is represented as red arrows.MOC images were used to have acloser look at the dark material andto analyse the dune shape.184,65 K193,29 K194,16 K206,40 K196,89 K176,78 K176,32 K159,81 K160,92 K187,01 K176,32 K159,81 K151,87 K178,14 KRecent and Fossil Deposits of Dark Materialin Martian CratersDaniela Tirsch1*, Ralf Jaumann1, Jörn Helbert1, Dennis Reiß1, Francois Forget2,Francois Poulet3 and Gerhard Neukum41Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany2Laboratoire de Météorologie Dynamique du CNRS, Université Paris 6, Paris3Institut d’Astrophysique Spatiale (IAS), Université Paris-Sud, Orsay Campus, Paris4Remote Sensing of the Earth and Planets, Free University Berlin, Germany* mail to: Daniela Tirsch@dlr.deFig. 1: Global overview of the 50 selected craters (background: MOLA shaded (DLR, ESA, FUB))Fig. 2: Extract from thereceived MCD data for thecraters of interest. Note thatthe crater names are inmany cases not the officialnames but only namesgiven here for this analysispointing at the geographicallocation.Fig. 7a: HRSC image of a barchan dune field in a crater at44.2°S, 303.3°E showing correlative wind directions(ESA/DLR/FUB).Fig. 8a: HRSC image of a barchan dune field in a crater at9.6°N, 150.1°E showing correlative wind directions(ESA/DLR/FUB).Fig. 9a: HRSC image of several barchan dunes in a craterat 14.3°S, 95.8°E showing correlative wind directions(ESA/DLR/FUB).Fig. 7b: THEMIS-BTR-mosaic with normalised temperaturesof the crater of fig. 7a. The absolute temperature of the dunefield is about 184 K (measured from I0613800).Fig. 8b: THEMIS-BTR-mosaic with normalised temperaturesof the crater of fig. 8a. The mean absolute temperature ofthe dune field is about 185 K (measured from I06168009).Fig. 9b: THEMIS-BTR-mosaic with normalised temperaturesof the crater of Fig. 9a. The mean absolute temperature ofthe dune field is about 196 K (measured from I06170007).Fig. 10a: HRSC image of a dune field in a crater at15.8°N, 181.5°E showing divergent wind directions(ESA/DLR/FUB).Fig. 11a: HRSC image of a barchan dune field in acrater at 25.8°N, 83.9°E showing opposite winddirections (ESA/DLR/FUB).Fig. 12a: HRSC image of a dune field in the FesenkovCrater showing divergent wind direct ions(ESA/DLR/FUB).Fig. 5: THEMIS mosaic of I04594022,I06816025, I0889007, I15128029 andI16950027. Bright colours indicate warmregions and dark colours indicate coldregions.References:[1] Edgett & Christensen (1994): Mars aeolian sand: Regional variations among dar-hued crater floor features.- JGR 99, E1, 1997 - 2018.[2] Forget et al. (1999): Improved general circulation models of the Martian atmosphere from the surface to above 80 km.- JRG 104, E10, 155-175.[3] Lewis et al. (1999): A climate database for Mars.- JRG 104, E10, 177-194.[4] Fenton et al. (2003): Aeolian processes in Proctor Crater on Mars: Sedimentary history as analyzed from multiple data sets.- JGR 108, E12, 1-39.[5] Jakosky et a.(2000): The thermal inertia of Mars from the Mars Global Surveyor Thermal Emission Spectrometer.- JGR 105, E4, 9643 - 9652.[6] Fenton & Mellon (2006): Thermal properties of sand from Thermal Emission Spectrometer (TES) andThermal Imaging System (THEMIS): Spatial variations within the Proctor Crater dune field on Mars.- JGR 111, E 06014, 7 p.[7] Stewart & Nimmo (2002): Surface runoff features on Mars: Testing the carbon dioxide formation hypothesis.- JGR 107, E9, 1-12.Fig. 3: Barchan dunes in a crater at 5°S, 344°EMars Express HRSC image, ESA/DLR/FUB)Fig. 4: MOC image E2200514 of the same dunesas shown in Fig. 3.In further analysis, the geographical distribution of mobile and fossil dune fields will be researched. For thisanalysis a bigger number of craters will be studied.Additionally, other wind direction data from the MarsGRAM model should be involved. The purpose for thisis to compare different data sets and to evaluate the reliability of the modelled data.Furthermore the thermal inertia of the dune surfaces should be calculated. This information can be used toestimate the grain size of a material [6].Fig. 10b: THEMIS-BTR mosaic of the crater of Fig. 10awith normalised temperatures.The absolute temperature of the dune field is 168 K - 176K(measured from I04594022).Fig. 11b: THEMIS-BTR mosaic of the crater of Fig. 11awith normalised temperatures.The absolute temperature of the dune field is 190 K - 195K(measured from I06707051).Fig. 12b: THEMIS-BTR mosaic of the crater of Fig. 12awith normalised temperatures.The mean absolute temperature of the dune field is about164 K (measured from I06663012).Fig. 6: THEMIS-BTR mosaic of I04594022,I06816025, I08289007 and I15128029.Fig. 14: Summarised results of the mobility analysis:20 of the 49 studied intra crater dunes are assumed to be mobile.13 of the craters could possess fossil dune fields.For the rest of the studied craters it was not possible to make a conclusion:It was either not possible to define the local wind direction or the THEMIS data show noobvious characteristic of the dark material.Fig. 13: Zoom into the Fesenkov Craterdune field showing barchan dunes(MOC image S05019074, highlystreched).

A climate database for Mars.-

a.(2000): The thermal inertia of Mars from the Mars Global Surveyor Thermal Emission Spectrometer.-

Aeolian processes in Proctor Crater on Mars: Sedimentary history as analyzed from multiple data sets.-

Improved general circulation models of the Martian atmosphere from the surface to above 80 km.-

Mars aeolian sand: Regional variations among dar-hued crater floor features.- JGR 99, E1,

Surface runoff features on Mars: Testing the carbon dioxide formation hypothesis.-

Thermal properties of sand from Thermal Emission Spectrometer (TES) andThermal Imaging System (THEMIS):

Recent and fossil deposits of dark material in Martian Craters

Recent and fossil deposits of dark material in Martian Craters

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