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dc.contributor.authorCui, J.
dc.contributor.authorYelle, R. V.
dc.contributor.authorZhao, L.-L.
dc.contributor.authorStone, S.
dc.contributor.authorJiang, F.-Y.
dc.contributor.authorCao, Y.-T.
dc.contributor.authorYao, M.-J.
dc.contributor.authorKoskinen, T. T.
dc.contributor.authorWei, Y.
dc.date.accessioned2018-03-13T23:58:28Z
dc.date.available2018-03-13T23:58:28Z
dc.date.issued2018-02-02
dc.identifier.citationThe Impact of Crustal Magnetic Fields on the Thermal Structure of the Martian Upper Atmosphere 2018, 853 (2):L33 The Astrophysical Journalen
dc.identifier.issn2041-8213
dc.identifier.doi10.3847/2041-8213/aaa89a
dc.identifier.urihttp://hdl.handle.net/10150/627044
dc.description.abstractUsing the Mars Atmosphere and Volatile Evolution Neutral Gas and Ion Mass Spectrometer data, we investigate the possible impact of crustal magnetic fields on the thermal structure of the Martian upper atmosphere. Our analysis reveals a clear enhancement in temperature over regions with strong crustal magnetic fields during two deep dip campaigns covering the periods of April 17-22 and September 2-8, both in 2015. Several controlling factors, such as solar EUV irradiance, relative atomic O abundance, and non-migrating tides, do not help to explain the observed temperature enhancement, and a magnetically driven scenario is favored. We evaluate the roles of several heating mechanisms that are likely modulated by the presence of crustal magnetic fields, including Joule heating, ion chemical heating, as well as electron impact heating via either precipitating solar wind electrons or locally produced photoelectrons. The respective heating rates of these mechanisms are substantially lower than the solar EUV heating rate, implying that none of them is able to interpret the observations.
dc.description.sponsorshipNational Science Foundation of China (NSFC) [41525015, 41774186, 41504133]; Science and Technology Development Fund of Macau SAR (FDCT) [039/2013/A2, 082/2015/A3]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/2041-8205/853/i=2/a=L33?key=crossref.df43887e5c08cd36a60720039c817737en
dc.rights© 2018. The American Astronomical Society. All rights reserved.en
dc.subjectplanets and satellites: individual (Mars)en
dc.titleThe Impact of Crustal Magnetic Fields on the Thermal Structure of the Martian Upper Atmosphereen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben
dc.identifier.journalThe Astrophysical Journal Lettersen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-13T22:40:14Z
html.description.abstractUsing the Mars Atmosphere and Volatile Evolution Neutral Gas and Ion Mass Spectrometer data, we investigate the possible impact of crustal magnetic fields on the thermal structure of the Martian upper atmosphere. Our analysis reveals a clear enhancement in temperature over regions with strong crustal magnetic fields during two deep dip campaigns covering the periods of April 17-22 and September 2-8, both in 2015. Several controlling factors, such as solar EUV irradiance, relative atomic O abundance, and non-migrating tides, do not help to explain the observed temperature enhancement, and a magnetically driven scenario is favored. We evaluate the roles of several heating mechanisms that are likely modulated by the presence of crustal magnetic fields, including Joule heating, ion chemical heating, as well as electron impact heating via either precipitating solar wind electrons or locally produced photoelectrons. The respective heating rates of these mechanisms are substantially lower than the solar EUV heating rate, implying that none of them is able to interpret the observations.


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