@article{
 title = {Surface age of the ice–dust mantle deposit in Malea Planum, Mars},
 type = {article},
 year = {2012},
 keywords = {Crater degradation,Icedust mantle,Malea Planum,Mars,Recent martian climate change},
 pages = {199-206},
 volume = {60},
 websites = {http://linkinghub.elsevier.com/retrieve/pii/S0032063311002625},
 month = {1},
 publisher = {Elsevier},
 day = {14},
 id = {75f3a8ea-090e-3023-a106-f5eec76558d3},
 created = {2012-01-12T03:08:19.000Z},
 accessed = {2012-01-12},
 file_attached = {true},
 profile_id = {b32caa3a-a6aa-3875-9eaa-ba9f1eb70905},
 last_modified = {2018-05-26T20:51:55.932Z},
 read = {true},
 starred = {false},
 authored = {true},
 confirmed = {true},
 hidden = {false},
 citation_key = {Willmes2012b},
 language = {en},
 notes = {<b>From Duplicate 1 ( </b><br/><br/><b><br/><i>Surface age of the ice–dust mantle deposit in Malea Planum, Mars</i><br/></b><br/><br/><b>- Willmes, Malte; Reiss, Dennis; Hiesinger, Harald; Zanetti, Michael )<br/><br/></b>},
 private_publication = {false},
 abstract = {The mid- and high-latitudes of Mars are covered by a smooth young mantle that is interpreted as an atmospherically derived air-fall deposit of ice and dust related to recent climate changes. In order to determine relative and absolute ages of this surface unit within the southern hemisphere, a systematic survey of all available HiRISE and CTX images in the Malea Planum region from 5560??S latitude and 5070??E longitude was performed and the distribution and the morphology of small impact craters on the mantle deposit were investigated. Using crater size-frequency measurements, we derived absolute model ages of ???35 Ma for the surface of the mantle, immediately south of the Hellas basin rim. Morphologic observations of the mantle, its fresh appearance, very low number of craters, and superposition on older units support this very young Amazonian age. Nearly all observed craters on the smooth mantle in Malea Planum are small and show signs of erosion, evidence for the ongoing modification of the ice-dust mantle. However, this modification has not been strong enough to reset the surface age. Compared to the ice-dust mantle at higher latitudes in the northern and southern hemisphere, the surface of the mantle in Malea Planum is older and thus has been relatively stable during obliquity changes in the last ???35 Ma. This is consistent with the hypothesis that the ice-dust mantle is a complex surface deposit of different layers, that shows a strong latitude dependence in morphology and has been deposited and degraded at different times in martian history. ?? 2011 Elsevier Ltd. All rights reserved.},
 bibtype = {article},
 author = {Willmes, Malte and Reiss, Dennis and Hiesinger, Harald and Zanetti, Michael},
 doi = {10.1016/j.pss.2011.08.006},
 journal = {Planetary and Space Science},
 number = {1}
}

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In order to determine relative and absolute ages of this surface unit within the southern hemisphere, a systematic survey of all available HiRISE and CTX images in the Malea Planum region from 5560??S latitude and 5070??E longitude was performed and the distribution and the morphology of small impact craters on the mantle deposit were investigated. Using crater size-frequency measurements, we derived absolute model ages of ???35 Ma for the surface of the mantle, immediately south of the Hellas basin rim. Morphologic observations of the mantle, its fresh appearance, very low number of craters, and superposition on older units support this very young Amazonian age. Nearly all observed craters on the smooth mantle in Malea Planum are small and show signs of erosion, evidence for the ongoing modification of the ice-dust mantle. However, this modification has not been strong enough to reset the surface age. Compared to the ice-dust mantle at higher latitudes in the northern and southern hemisphere, the surface of the mantle in Malea Planum is older and thus has been relatively stable during obliquity changes in the last ???35 Ma. This is consistent with the hypothesis that the ice-dust mantle is a complex surface deposit of different layers, that shows a strong latitude dependence in morphology and has been deposited and degraded at different times in martian history. ?? 2011 Elsevier Ltd. All rights reserved.","bibtype":"article","author":"Willmes, Malte and Reiss, Dennis and Hiesinger, Harald and Zanetti, Michael","doi":"10.1016/j.pss.2011.08.006","journal":"Planetary and Space Science","number":"1","bibtex":"@article{\n title = {Surface age of the ice–dust mantle deposit in Malea Planum, Mars},\n type = {article},\n year = {2012},\n keywords = {Crater degradation,Icedust mantle,Malea Planum,Mars,Recent martian climate change},\n pages = {199-206},\n volume = {60},\n websites = {http://linkinghub.elsevier.com/retrieve/pii/S0032063311002625},\n month = {1},\n publisher = {Elsevier},\n day = {14},\n id = {75f3a8ea-090e-3023-a106-f5eec76558d3},\n created = {2012-01-12T03:08:19.000Z},\n accessed = {2012-01-12},\n file_attached = {true},\n profile_id = {b32caa3a-a6aa-3875-9eaa-ba9f1eb70905},\n last_modified = {2018-05-26T20:51:55.932Z},\n read = {true},\n starred = {false},\n authored = {true},\n confirmed = {true},\n hidden = {false},\n citation_key = {Willmes2012b},\n language = {en},\n notes = {<b>From Duplicate 1 ( </b><br/><br/><b><br/><i>Surface age of the ice–dust mantle deposit in Malea Planum, Mars</i><br/></b><br/><br/><b>- Willmes, Malte; Reiss, Dennis; Hiesinger, Harald; Zanetti, Michael )<br/><br/></b>},\n private_publication = {false},\n abstract = {The mid- and high-latitudes of Mars are covered by a smooth young mantle that is interpreted as an atmospherically derived air-fall deposit of ice and dust related to recent climate changes. 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Compared to the ice-dust mantle at higher latitudes in the northern and southern hemisphere, the surface of the mantle in Malea Planum is older and thus has been relatively stable during obliquity changes in the last ???35 Ma. This is consistent with the hypothesis that the ice-dust mantle is a complex surface deposit of different layers, that shows a strong latitude dependence in morphology and has been deposited and degraded at different times in martian history. ?? 2011 Elsevier Ltd. 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