2009/06/04 by Lixin Dai, Steven V. Fuerst, R. D. Blandford +1 · 2 citations
Engineering · Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Flare #Galactic Center #Galaxy #Mechanics and Biomechanics Studies #Orbit (dynamics) #Physics #Pulsars and Gravitational Waves Research #Quasi periodic #Solar flare #Stars #Supermassive black hole #astro-ph.HE
paper · pdf · doi:10.1111/j.1365-2966.2009.16038.x
16 pages, 11 figures, submitted to MNRAS; corrected typos
arxiv created 2009/06/04 · openalex publication_date 2010/01/15 · arxiv updated 2015/05/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present simulated results of quasi-periodic flares generated by the inelastic collisions of a star bound to a supermassive black hole and its attendant accretion disc. We show that the behaviour of the quasi-periodicity is affected by the mass and spin of the black hole and the orbital elements of the stellar orbit. We also evaluate the possibility of extracting useful information on these parameters and verifying the character of the Kerr metric from such quasi-periodic signals. Comparisons are made with the observed optical outbursts of OJ 287, infrared flares from the Galactic Centre and X-ray variability in RE J1034+396.