Statistics – Computation
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994p%26ss...42..677p&link_type=abstract
Planetary and Space Science (ISSN 0032-0633), vol. 42, no. 8, p. 677-683
Statistics
Computation
2
Computational Astrophysics, Equations Of Motion, Fireballs, Gravitational Effects, Meteoroids, Orbital Mechanics, Solar Orbits, Approximation, Azimuth, Diurnal Variations, Two Body Problem, Velocity Distribution
Scientific paper
The classical method of the determination of the orbital elements of meteoroids is based on a sequence of corrections applied to the velocity vector of an observed meteor. The main aim of such an approach is the determination of the meteoroid's motion under the gravitational influence of the Sun but we are able to observe this motion only under the additional influence of the Earth. The classical method treats this switch from the Earth's gravitational center to the solar one as the process tacitly assumes that the size of the gravitational sphere of influence of the Earth is negligible as compared with the size of this sphere of the Sun. Assuming on the contrary to this classical method that the time of the passage is infinite, we should follow the meteoroid motion continuously in time from the moment of its apparition backwards to the moment the Sun's gravitational influence surely dominates. To do so, we have numerically integrated the equations of motion of meteoroids under the simultaneous action both of the Sun and the Earth from their time of the appearance in the atmosphere back to the moment the meteoroid-Earth distance reached at least 107km to ensure the body as well outside the sphere of activity of the Earth. In order to visualize the differences we have used the precise data of 17 fireballs photographed by the European fireball network. We can also draw the general conclusion that the slower the meteoroid the smaller is its eccentricity, as well as the semimajor axis as compared with their classical values.
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