The resistive effect of the solar wind on the orbits of solid bodies in the solar system

Details The resistive effect of the solar wind on the orbits of solid bodies in the solar system The resistive effect of the solar wind on the orbits of solid bodies in the solar system

Aug 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977mnras.180..289d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 180, Aug. 1977, p. 289-296. Research supported by the Science Research

Astronomy and Astrophysics

Astronomy

5

Cosmology, Planetary Evolution, Solar Orbits, Solar System, Solar Wind, Stellar Evolution, Angular Momentum, Astronomical Models, Celestial Mechanics, Equations Of Motion, T Tauri Stars

Scientific paper

An equation of motion for a body orbiting the sun and moving through a radially flowing solar wind is derived under the assumption that the body does not accrete any significant amount of matter. An exact analytical solution is obtained by assuming that the wind velocity is much greater than the body's orbital velocity. The results are applied to the terrestrial planets, asteroids, meteorites, and interplanetary grains for the cases of the present solar wind and the enhanced wind existing during the sun's T Tauri phase. It is shown that: (1) the resistive effect due to solar radiation dominates that of the solar wind for all solid objects in the solar system at the present time; (2) the solar wind would have been the dominant resistive agent in the past; (3) the solar-wind effect on the terrestrial planets and large asteroids would have been small during the T Tauri phase; (4) smaller asteroids would have undergone substantial rounding at that time; and (5) the meteoritic material now observed is not primordial but was produced subsequent to the T Tauri phase.

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