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dc.contributor.authorStevens, M. H.
dc.contributor.authorSiskind, D. E.
dc.contributor.authorEvans, J. S.
dc.contributor.authorJain, Sonal K.
dc.contributor.authorSchneider, N. M.
dc.contributor.authorDeighan, J.
dc.contributor.authorStewart, A. I. F.
dc.contributor.authorCrismani, M.
dc.contributor.authorStiepen, A.
dc.contributor.authorChaffin, M. S.
dc.contributor.authorMcClintock, W. E.
dc.contributor.authorHolsclaw, G. M.
dc.contributor.authorLefèvre, F.
dc.contributor.authorLo, D. Y.
dc.contributor.authorClarke, J. T.
dc.contributor.authorMontmessin, F.
dc.contributor.authorJakosky, B. M.
dc.date.accessioned2017-07-27T19:43:47Z
dc.date.available2017-07-27T19:43:47Z
dc.date.issued2017-05-28
dc.identifier.citationMartian mesospheric cloud observations by IUVS on MAVEN: Thermal tides coupled to the upper atmosphere 2017, 44 (10):4709 Geophysical Research Lettersen
dc.identifier.issn00948276
dc.identifier.doi10.1002/2017GL072717
dc.identifier.urihttp://hdl.handle.net/10150/624978
dc.description.abstractWe report observations of Martian mesospheric ice clouds and thermospheric scale heights by the Imaging Ultraviolet Spectrograph on NASA's Mars Atmosphere and Volatile Evolution mission. The clouds are observed between 6A.M. and 8A.M. local time using mid-UV limb observations between 60 and 80km tangent altitude where ice particles that scatter sunlight can appear as detached layers near the equator. The equatorial longitudinal distribution shows populations of clouds near -110 degrees E and -10 degrees E as well as a population near 90 degrees E, which does not have a clear precedent. The cloud populations indicate a wave 3 pattern near 70km, which is confirmed by independent mesospheric temperature observations. Scale heights 100km above the clouds derived from concurrent Imaging Ultraviolet Spectrograph (IUVS) observations also reveal a wave 3 longitudinal structure, suggesting that the temperature oscillations enabling the formation of mesospheric clouds couple to the upper atmosphere. Plain Language Summary The manuscript describes the observation of Martian mesospheric clouds between 60 and 80km altitude by the Imaging Ultraviolet Spectrograph (IUVS) on NASA's MAVEN spacecraft. The cloud observations are uniquely obtained at early morning local times, which complement previous observations obtained primarily later in the diurnal cycle. Differences in the geographic distribution of the clouds from IUVS observations indicate that the local time is crucial for the interpretation of mesospheric cloud formation. We also report concurrent observations of upper atmospheric scale heights near 170 km altitude, which are diagnostic of temperature. These observations suggest that the dynamics enabling the formation of mesospheric clouds propagate all the way to the upper atmosphere.
dc.description.sponsorshipNASA through the Mars Exploration Program; NASA MAVEN Participating Scientist programen
dc.language.isoenen
dc.publisherAMER GEOPHYSICAL UNIONen
dc.relation.urlhttp://doi.wiley.com/10.1002/2017GL072717en
dc.rights©2017. American Geophysical Union. All Rights Reserved. This article has been contributed to by US Government employees and their work is in the public domain in the USA.en
dc.subjectMarsen
dc.subjectmesosphereen
dc.subjectcloudsen
dc.subjecttidesen
dc.subjecttemperatureen
dc.titleMartian mesospheric cloud observations by IUVS on MAVEN: Thermal tides coupled to the upper atmosphereen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben
dc.identifier.journalGeophysical Research Lettersen
dc.description.note6 month embargo; First published: 28 May 2017en
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
dc.contributor.institutionSpace Science Division, Naval Research Laboratory; Washington District of Columbia USA
dc.contributor.institutionSpace Science Division, Naval Research Laboratory; Washington District of Columbia USA
dc.contributor.institutionComputational Physics, Inc.; Springfield Virginia USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratoire de Physique Atmosphérique et Planétaire, Space Sciences, Technologies and Astrophysics Research Institute; Université de Liége; Liége Belgium
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
dc.contributor.institutionLATMOS, CNRS/UPMC/UVSQ; Paris France
dc.contributor.institutionLunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
dc.contributor.institutionCenter for Space Physics; Boston University; Boston Massachusetts USA
dc.contributor.institutionLATMOS, CNRS/UPMC/UVSQ; Paris France
dc.contributor.institutionLaboratory for Atmospheric and Space Physics; Boulder Colorado USA
refterms.dateFOA2017-11-29T00:00:00Z
html.description.abstractWe report observations of Martian mesospheric ice clouds and thermospheric scale heights by the Imaging Ultraviolet Spectrograph on NASA's Mars Atmosphere and Volatile Evolution mission. The clouds are observed between 6A.M. and 8A.M. local time using mid-UV limb observations between 60 and 80km tangent altitude where ice particles that scatter sunlight can appear as detached layers near the equator. The equatorial longitudinal distribution shows populations of clouds near -110 degrees E and -10 degrees E as well as a population near 90 degrees E, which does not have a clear precedent. The cloud populations indicate a wave 3 pattern near 70km, which is confirmed by independent mesospheric temperature observations. Scale heights 100km above the clouds derived from concurrent Imaging Ultraviolet Spectrograph (IUVS) observations also reveal a wave 3 longitudinal structure, suggesting that the temperature oscillations enabling the formation of mesospheric clouds couple to the upper atmosphere. Plain Language Summary The manuscript describes the observation of Martian mesospheric clouds between 60 and 80km altitude by the Imaging Ultraviolet Spectrograph (IUVS) on NASA's MAVEN spacecraft. The cloud observations are uniquely obtained at early morning local times, which complement previous observations obtained primarily later in the diurnal cycle. Differences in the geographic distribution of the clouds from IUVS observations indicate that the local time is crucial for the interpretation of mesospheric cloud formation. We also report concurrent observations of upper atmospheric scale heights near 170 km altitude, which are diagnostic of temperature. These observations suggest that the dynamics enabling the formation of mesospheric clouds propagate all the way to the upper atmosphere.


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