HST/Stis Observations Of The D/H Ratio In The Martian Upper Atmosphere

Details HST/Stis Observations Of The D/H Ratio In The Martian Upper Atmosphere HST/Stis Observations Of The D/H Ratio In The Martian Upper Atmosphere

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6013c&link_type=abstract

American Astronomical Society, DPS meeting #38, #60.13; Bulletin of the American Astronomical Society, Vol. 38, p.600

Astronomy and Astrophysics

Astronomy

Scientific paper

The present-day D/H ratio gives vital information needed to understand the evolution of Mars' atmosphere, the historic escape of water into space, and potentially the remaining water abundance on Mars. Since this ratio appears to vary with altitude in the martian atmosphere, it is important to determine the value in the upper atmosphere, from which D and H may escape into space. HST observations of Mars from May 2001 used the STIS echelle spectrograph in a novel long-aperture mode, allowing spatially resolved (0.1 arc sec) high resolution (0.0055 nm) spectra across the entire martian disc and upper atmosphere. The novel observing mode is now fully calibrated, and we will present values for the D and H densities and the D/H ratio based on comparison of the data with two independent radiative transfer codes. The codes are presently being run to derive the H density from comparison of the optically thick spectra line profile and the brightness distribution across the martian disc and onto the sky. This work was supported by grant HST-GO-08658.05-A from the Space Telescope Science Institute to Boston University.

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