2000/02/29 by Shai Ayal, S. Ayal, Mario Livio +3 · 5 citations
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Experimental and Theoretical Physics Studies #Galaxy #Intermediate-mass black hole #Physics #Pulsars and Gravitational Waves Research #Solar mass #Star (game theory) #Supermassive black hole #Supernova #astro-ph #gr-qc #physics.comp-ph
paper · pdf · doi:10.1086/317835
published as Astrophys.J. 545 (2000) 772-780 · 19 pages, 13 figures, Revised version as accepted by ApJ. High resolution figures available at http://merger.phys.huji.ac.il/~shai/last_pages.ps.gz (1.2 MB)
openalex publication_date 2000/12/20 · arxiv created 2000/12/24 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We study the long-term evolution of a solar-type star that is being disrupted by a supermassive (10 6 M ☉ ) black hole. The evolution is followed from the disruption event, which turns the star into a long, thin stream of gas, to the point at which some of this gas returns to pericenter and begins its second orbit around the black hole. Following the evolution for this long allows us to determine the amount of mass that is accreted by the black hole. We find that approximately 75% of the returning mass is not accreted but instead becomes unbound, following the large compression characterizing the return to pericenter. The impact of a tidal disruption on the surrounding gas may therefore be like that of two consecutive supernova-type events.