Mathematics
Scientific paper
Sep 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001phdt........69g&link_type=abstract
PhD Thesis, Faculty of Mathematics and Physics, University in Ljubljana, Jadranska 19, 1000 Ljubljana, Slovenia
Mathematics
9
Black Holes, Numerical Relativity, Relativity And Gravitation
Scientific paper
I present the study of rapid luminosity changes due to interaction of a source with the black hole. By numerically simulating a source and its motion in the gravitational field near the black hole I calculate its apparent luminosity by tracing light-rays in curved space-time from a source to the distant observer. Two model sources were considered: (1) a point like source, applying to cases of a light source being much smaller than the black hole. Such possible astrophysical scenarios include: an orbiting blob in accretion disk about a central black hole in active galactic nuclei, a solar type star falling into a giant black hole (MBH>108 Modot) or the infall of small debris into a possible black hole in gamma ray burstars. (2) a model star, comparable in size to the black hole, applying to cases such as a solar type star interacting with about 106 Modot black hole. Results of simulations show that variations in luminosity occur on typical timescales of a few M to a few 100 M, where M=GMBH/c3. For a 106Modot black hole these correspond from sim 5 s to sim 10 min, and for a 1010 Modot black hole to time spans of sim 10 hours to a few months. Results in the case of the point like model (1) show that the maximum luminosity variations are about 20 times the original luminosity. In case (2) the outcome of the stellar encounter with the black hole strongly depends on the stellar angular momentum with respect to the black hole. Stars with small angular momentum are completely swallowed by the black hole, while stars with high angular momentum experience only slight tidal distortion and luminosity changes. The most dramatic is the encounter with critical angular momentum, during which the star is sheared into the long thin spiral. The exposure of the hot interior results in a sudden release of a very large fraction of stellar internal energy, up to 1041 J for a solar type star, as suggested by these results.
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