Open AccessZonal variations of peak ionization rates in upper atmosphere of Mars at high latitude using Mars Global Surveyor accelerometer data
Author(s) -
Seth S. P.,
Brahmananda Rao V.,
Esprito Santo C. M.,
Haider S. A.,
Choksi V. R.
Publication year - 2006
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2006ja011753
Subject(s) - mars exploration program , atmosphere of mars , atmospheric sciences , scale height , atmosphere (unit) , thermosphere , latitude , environmental science , ionosphere , geology , physics , martian , geodesy , meteorology , astronomy
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 F 10.7 ∼ 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 CO 2 + , N 2 + 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 CO 2 + , N 2 + , 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.