Zonal variations of peak ionization rates in upper atmosphere of Mars at high latitude using Mars Global Surveyor accelerometer data

Details Zonal variations of peak ionization rates in upper atmosphere of Mars at high latitude using Mars Global Surveyor accelerometer data Zonal variations of peak ionization rates in upper atmosphere of Mars at high latitude using Mars Global Surveyor accelerometer data

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jgra..11109308s&link_type=abstract

Journal of Geophysical Research, Volume 111, Issue A9, CiteID A09308

Physics

Geophysics

9

Ionosphere: Ionization Processes (7823), Ionosphere: Wave Propagation (0689, 3285, 4275, 4455, 6934), Mathematical Geophysics: Fourier Analysis (3255), Atmospheric Processes: Tides And Planetary Waves

Scientific paper

The Accelerometer Experiment onboard Mars Global Surveyor (MGS) measured many density profiles in the upper atmosphere of Mars during aerobraking at many latitudes, longitudes, altitudes, local solar time (LST), and seasons. Here, in this paper, we use the accelerometer data of 57 orbits (P0588-P0648) from 30 September 1998 to 24 October 1998 between latitude ranges (50°-70°N) at LST 1600 hours, under spring equinox and medium solar activity conditions (average F10.7 ~ 120). Using these densities, the neutral densities of different gases are derived from their mixing ratio. From these neutral densities the longitudinal distribution of peak photoionization rates, peak photoelectron impact ionization rates, and the total peak ionization rates of CO2+, N2+ and O+ are obtained for solar zenith angle 78° at wavelength range 10-1025.7 Å due to solar EUV radiation using analytical yield spectrum approach (AYS). These calculations are made at different altitudes and longitudes starting from 115 to 220 km and 0° to 360°E using intervals of 0.1 km and 5°, respectively. These conditions are appropriate for MGS phase 2 aerobraking period from which the accelerometer data are used. The Fourier analysis of the various peak ionization rates of CO2+, N2+, and O+ indicates the presence of two dominant harmonic regions at high latitude in the upper atmosphere of Mars. The first is a class of long planetary-scale waves that may be associated with the fixed topography of Martian surface. The second is a class of rapidly moving transient disturbances that may be associated with baroclinic instability processes.

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