The tidal disruption of a star by a massive black hole

Details The tidal disruption of a star by a massive black hole The tidal disruption of a star by a massive black hole

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...346l..13e&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 346, Nov. 1, 1989, p. L13-L16.

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137

Active Galactic Nuclei, Black Holes (Astronomy), Hydrodynamic Equations, Main Sequence Stars, Stellar Mass, Computational Astrophysics, Galactic Clusters, Stellar Luminosity

Scientific paper

Results are reported from a three-dimensional numerical calculation of the tidal disruption of a low-mass main-sequence star on a parabolic orbit around a massive black hole (Mh = 10 to the 6th stellar mass). The postdisruption evolution is followed until hydrodynamic forces becomes negligible and the liberated gas becomes ballistic. Also given is the rate at which bound mass returns to pericenter after orbiting the hole once. The processes that determine the time scale to circularize the debris orbits and allow an accretion torus to form are discussed. This time scale and the time scales for radiative cooling and accretion inflow determine the onset and duration of the subsequent flare in the AGN luminosity.

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