Abstract
The dynamical interaction of small interplanetary particles with the Martian upper atmosphere is considered. The equation of motion of a small particle, entering the Martian atmosphere with cosmic velocity, is integrated numerically in a general form for three Martian model atmospheres. The results of the numerical integrations are compared with similar computations carried out for the Earth's upper atmosphere. While in the case of the Earth, the EBH (Effective Braking Height) is around 90 km, the different Martian density profiles yield EBH of 105, 80, and 65 km for the models suggested by Chamberlain and McElroy, Donahue, and Johnson, respectively. A preliminary examination of the first photograph taken by Mariner IV during its Martian flyby, which reveals the existence of light-scattering particles in the Martian upper atmosphere at altitudes of over 100 km, suggests that Chamberlain and McElroy's density profile is the most probable of the three.
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