Burgdorf, M., Encrenaz, Th., Lellouch, E., Feuchtgruber, H., Davis, G. R., Swinyard, B. M., de Graauw, Th., Morris, P. W., Sidher, S. D., Griffin, Matthew Joseph ![]() |
Abstract
Infrared spectra of Mars were taken with the two complementary spectrometers onboard the European Space Agency's Infrared Space Observatory (ISO), in both moderate- and high-resolution mode. From the strengths of the observed water lines we derived information about the vertical distribution of water vapor and on the emissivity of the dust/surface system in the infrared. Assuming atmospheric and surface temperatures derived from the European Martian Climate Database with a slight adjustment to the observed 15-μm CO2 band, the ISO data are consistent with an H2O mixing ratio of (3±1)×10−4 at the surface, a saturation level at 13±2 km, and a total column density of 12±3.5 pr-μm. The mean disk emissivity is found to be close to 1.0 at 6 μm and 0.92±0.02 at 40 μm. At longer wavelengths the emissivity decreases from a value of 0.97±0.03 at 50μm to 0.92±0.03 at 180 μm.
Item Type: | Article |
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Date Type: | Publication |
Status: | Published |
Schools: | Physics and Astronomy |
Subjects: | Q Science > QB Astronomy |
Publisher: | Elsevier Science |
ISSN: | 0019-1035 |
Last Modified: | 18 Oct 2022 12:40 |
URI: | https://orca.cardiff.ac.uk/id/eprint/10911 |
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