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Martian mesospheric cloud observations by IUVS on MAVEN: Thermal tides coupled to the upper atmosphere
Author(s) -
Stevens M. H.,
Siskind D. E.,
Evans J. S.,
Jain S. K.,
Schneider N. M.,
Deighan J.,
Stewart A. I. F.,
Crismani M.,
Stiepen A.,
Chaffin M. S.,
McClintock W. E.,
Holsclaw G. M.,
Lefèvre F.,
Lo D. Y.,
Clarke J. T.,
Montmessin F.,
Jakosky B. M.
Publication year - 2017
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1002/2017gl072717
Subject(s) - atmosphere of mars , martian , atmosphere (unit) , atmospheric sciences , equator , mars exploration program , population , geology , astrobiology , environmental science , latitude , physics , astronomy , meteorology , demography , sociology
Abstract We 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 6 A.M. and 8 A.M. local time using mid‐UV limb observations between 60 and 80 km 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°E and −10°E as well as a population near 90°E, which does not have a clear precedent. The cloud populations indicate a wave 3 pattern near 70 km, which is confirmed by independent mesospheric temperature observations. Scale heights 100 km 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.