2008/11/30 by James Guillochon, Enrico Ramirez-Ruiz, E. Ramírez-Ruiz +2 · 108 citations
Engineering · Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Gamma-ray bursts and supernovae #Mechanics and Biomechanics Studies #Observable #Orbit (dynamics) #Physics #RADIUS #Stars #astro-ph
paper · pdf · doi:10.1088/0004-637x/705/1/844
published in The Astrophysical Journal 705(1), 844-853 (IOP Publishing) · 10 pages, 7 figures, Accepted to ApJ. For movies see http://www.ucolick.org/~jfg/2008a.html
arxiv created 2009/09/17 · openalex publication_date 2009/10/15 · arxiv updated 2015/05/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We describe a three-dimensional simulation of a 1 M ☉ solar-type star approaching a 10 6 M ☉ black hole on a parabolic orbit with a pericenter distance well within the tidal radius. While falling toward the black hole, the star is not only stretched along the orbital direction but also even more severely compressed at right angles to the orbit. The overbearing degree of compression achieved shortly after pericenter leads to the production of strong shocks that largely homogenize the temperature profile of the star, resulting in surface temperatures comparable to the initial temperature of the star's core. This phenomenon, which precedes the fallback accretion phase, gives rise to a unique double-peaked X-ray signature that, if detected, may be one of the few observable diagnostics of how stars behave under the influence of strong gravitational fields. If ∼10 6 M ☉ black holes were prevalent in small or even dwarf galaxies, the nearest of such flares may be detectable by EXIST from no further away than the Virgo Cluster.