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Martian Meteor Ionization LayersSmall interplanetary grains bombard Mars, like all the solar system planets, and, like all the planets with atmospheres, meteoric ion and atom layers form in the upper atmosphere. We have developed a comprehensive one-dimensional model of the Martian meteoric ionization layer including a full chemical scheme. A persistent layer of magnesium ions should exist around an altitude of 70 km. Unlike the terrestrial case, where the metallic ions are formed via charge-exchange with the ambient ions, Mg(+) in the Martian atmosphere is produced by photoionization. Nevertheless, the predicted metal layer peak densities for Earth and Mars are similar. Diffusion solutions, such as those presented here, should be a good approximation of the metallic ions in regions where the magnetic field is negligible and may provide a significant contribution to the nightside ionosphere. The low ultraviolet absorption of the Martian atmosphere may make Mars an excellent laboratory in which to study meteoric ablation. Resonance lines not seen in the spectra of terrestrial meteors may be visible to a surface observatory in the Martian highlands.
Document ID
19990080907
Acquisition Source
Goddard Space Flight Center
Document Type
Reprint (Version printed in journal)
Authors
Grebowsky, J. M.
(NASA Goddard Space Flight Center Greenbelt, MD United States)
Pesnell, W. D.
(Nomad Research, Inc. Bowie, MD United States)
Date Acquired
August 19, 2013
Publication Date
January 1, 1999
Subject Category
Lunar And Planetary Exploration
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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