Small Scale Wave Structures in the Martian Atmosphere as seen by the Radio Science Experiment MaRS on Mars Express

Details Small Scale Wave Structures in the Martian Atmosphere as seen by the Radio Science Experiment MaRS on Mars Express Small Scale Wave Structures in the Martian Atmosphere as seen by the Radio Science Experiment MaRS on Mars Express

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p24a..04t&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P24A-04

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[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [0350] Atmospheric Composition And Structure / Pressure, Density, And Temperature, [6969] Radio Science / Remote Sensing

Scientific paper

The Radio Science Experiment MaRS on Mars Express is sounding the Martian atmosphere and ionosphere using the spacecraft radio subsystem. A simultaneous and coherent dual-frequency downlink at X- and S-band via the Spacecraft's High Gain Antenna (HGA) is required to separate effects of dispersive media from the classical Doppler shift. Vertical profiles of pressure, temperature and density in the neutral atmosphere can be derived with an altitude resolution of only a few hundred metres. The high vertical resolution of the MaRS temperature profiles provides the unique opportunity to study small scale vertical wave structures in the Martian lower atmosphere between the surface and about 40 km. Several of these small scale temperature perturbations are caused by gravity waves (buoyancy waves) induced by atmospheric processes like topographical forcing, convection, or wind shear. Gravity waves play a significant role in the energy and momentum budget of the Earth and comparable important effects are also predicted for Mars. Observations of vertical small scale gravity waves on Mars are still sparse on the other hand. The small scale temperature perturbations with vertical wavelengths smaller than 10 kilometres are examined to investigate the global distribution and seasonal variability of gravity wave energy on Mars. Comparisons with other independent measurements and model predictions will be shown.

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