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Nonmigrating tides in the Martian atmosphere as observed by MAVEN IUVS
Author(s) -
Lo Daniel Y.,
Yelle Roger V.,
Schneider Nicholas M.,
Jain Sonal K.,
Stewart A. Ian F.,
England Scott L.,
Deighan Justin I.,
Stiepen Arnaud,
Evans J. Scott,
Stevens Michael H.,
Chaffin Michael S.,
Crismani Matteo M. J.,
McClintock William E.,
Clarke John T.,
Holsclaw Gregory M.,
Lefèvre Franck,
Jakosky Bruce M.
Publication year - 2015
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 - 10.1002/2015gl066268
Subject(s) - atmospheric tide , martian , mars exploration program , middle latitudes , equator , geology , atmosphere (unit) , atmospheric sciences , atmosphere of mars , planet , amplitude , altitude (triangle) , astrobiology , latitude , ionosphere , geophysics , thermosphere , meteorology , geodesy , physics , astronomy , geometry , mathematics , quantum mechanics
Abstract Using the Mars Atmospheric and Volatile EvolutioN mission (MAVEN) Imaging Ultraviolet Spectrograph (IUVS), we found periodic longitudinal variations in CO 2 density in the Martian atmosphere. These density variations are derived from observations of theCO 2 +( B 2Σ + → X 2 Π ) emission from limb scans in the 100–190 km altitude range. The variations exhibit significant structure with longitudinal wave numbers 1, 2, and 3 in an effectively constant local solar time frame, and we attribute this structure to nonmigrating tides. The wave‐2 component is dominated by the diurnal eastward moving DE1 tide at the equator and the semidiurnal stationary S0 tide at the midlatitudes. Wave‐3 is dominated by the diurnal eastward moving DE2 tide, with possibly the semidiurnal eastward moving SE1 tide causing an amplitude increase at the midlatitudes. Structure in the wave‐1 component can be explained by the semidiurnal westward moving SW1 tide.