| Literature DB >> 31031414 |
Hannah C M Susorney1,2, Peter B James3, Catherine L Johnson1,2, Nancy L Chabot4, Carolyn M Ernst4, Erwan M Mazarico5, Gregory A Neumann5, Mallory L Kinczyk6.
Abstract
The discovery of Mercury's radar-bright deposits has expanded our understanding of volatiles in the solar system. Key to deciphering the history and origin of the radar-bright deposits is an estimate of the volume of radar-bright material that in turn requires a measure of the average thickness of the deposits. In this study we investigate changes in topography across radar-bright deposits hosted in flat-floored, complex craters using individual edited Mercury Laser Altimeter (MLA) tracks. We compare the difference in heights of radar-bright regions and non-radar-bright regions of the crater floor and the difference of similarly sized and located regions in non-radar-bright craters and show that the two populations cannot be distinguished. The similarity of topography in these two sets of craters allows an upper limit of 15 m to be placed on the thickness of the radar-bright deposits.Entities:
Keywords: Laser Altimeter; Mercury; Polar Deposits
Year: 2019 PMID: 31031414 PMCID: PMC6480407 DOI: 10.1016/j.icarus.2019.01.016
Source DB: PubMed Journal: Icarus ISSN: 0019-1035 Impact factor: 3.508