The passage of a star by a massive black hole

Details The passage of a star by a massive black hole The passage of a star by a massive black hole

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..377n&link_type=abstract

Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 377-385.

Astronomy and Astrophysics

Astronomy

35

Black Holes (Astronomy), Equations Of Motion, Stellar Motions, Stellar Oscillations, Stellar Rotation, Active Galactic Nuclei, Angular Momentum, Astrodynamics, Equations Of State, Hydrodynamics, Particle Motion, Quasars, Stellar Mass, X Ray Sources

Scientific paper

The gridless, smoothed particle hydrodynamic method of Lucy (1977) and Gingold and Monaghan (1977, 1980, a, b, 1981) is used to solve the three-dimensional problem posed by the effects on a 1.0 solar mass star of a 10,000 solar mass black hole's passage, in an initially parabolic orbit with a variety of pericenter distances. It is found that the tidal forces induce rotation and radial and nonradial pulsations in the star, and that the loss of orbital energy to these internal motions leads to the star's capture by the black hole. While the outer layers of the star are disrupted at small pericenter distances, the entire star is destroyed at even smaller distances. These results are applicable to X-ray sources, active galactic nuclei, and quasars

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