Principal modes of variability of Martian atmospheric surface pressure

Details Principal modes of variability of Martian atmospheric surface pressure Principal modes of variability of Martian atmospheric surface pressure

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003georl..30m..40l&link_type=abstract

Geophysical Research Letters, Volume 30, Issue 13, pp. 40-1, CiteID 1707, DOI 10.1029/2002GL015909

Other

1

Global Change: Atmosphere (0315, 0325), Global Change: Climate Dynamics (3309), Meteorology And Atmospheric Dynamics: Planetary Meteorology (5445, 5739), Planetary Sciences: Atmospheres-Structure And Dynamics

Scientific paper

An analysis of daily-to-interannual variability in the surface pressure field of the Martian nothern hemisphere as given by a Martian climate model is presented. In an empirical orthogonal function (EOF) decomposition, the dominant first two modes of variability comprise a zonal wavenumber 1 feature centered at 70 N latitude moving eastward with a period of 6 to 8 sols. This feature is a baroclinic wave and accounts for 53% of the northern hemisphere non-stationary surface pressure variability, and, when active, has an amplitude of up to 2% of local surface pressure. The third mode of the EOF decomposition is annular about the Martian north pole, is null southward of 70 N, and accounts for 7% of the northern hemisphere non-stationary surface pressure variability. The baroclinic wave (EOFs 1 & 2) is active during northern hemisphere winter and spring, consistent with models of the Martian atmospheric circulation, and the annular mode (EOF 3) is active only at the onset and demise of the baroclinic feature. When active, it is not uncommon for the annular mode to reside in either its positive or negative state stably for 20 to 30 sols. It is postulated that baroclinic waves with longitudinal wavenumber 2, 3, and 4 act as a pump for the annular mode. The annular mode should not be present in MGS TES data.

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