1. The fine line between total and partial tidal disruption events
- Author
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Alessandro Lupi, Sergio Campana, Enrico Ramirez-Ruiz, Deborah Mainetti, Monica Colpi, James Guillochon, Eric R. Coughlin, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ITA, USA, FRA, Mainetti, D, Lupi, A, Campana, S, Colpi, M, Coughlin, E, Guillochon, J, Ramirez Ruiz, E, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
Critical distance ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Astrophysics::High Energy Astrophysical Phenomena ,black hole physics ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Star (graph theory) ,Fine line ,01 natural sciences ,methods: numerical ,Black hole physic ,General Relativity and Quantum Cosmology ,Accretion, accretion disk ,Accretion disc ,accretion ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Finite mass ,Astrophysics::Galaxy Astrophysics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Accretion ,accretion disks ,Black hole physics ,Galaxies: nuclei ,Hydrodynamics ,Methods: numerical ,Astronomy and Astrophysics ,Space and Planetary Science ,Accretion (meteorology) ,010308 nuclear & particles physics ,Hydrodynamic ,Astronomy and Astrophysic ,Galaxy ,Polytrope ,hydrodynamics ,Astrophysics::Earth and Planetary Astrophysics ,galaxies: nuclei ,Astrophysics - High Energy Astrophysical Phenomena ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Flares from tidal disruption events are unique tracers of quiescent black holes at the centre of galaxies. The appearance of these flares is very sensitive to whether the star is totally or partially disrupted, and in this paper we seek to identify the critical distance of the star from the black hole (r_d) that enables us to distinguish between these two outcomes. We perform here Mesh-free Finite Mass, traditional, and modern Smoothed Particle Hydrodynamical simulations of star-black hole close encounters, with the aim of checking if the value of r_d depends on the simulation technique. We find that the critical distance (or the so-called critical disruption parameter beta_d) depends only weakly on the adopted simulation method, being beta_d=0.92\pm 0.02 for a gamma=5/3 polytrope and beta_d=2.01\pm 0.01 for a gamma=4/3 polytrope., 8 pages, 8 figures, 2 tables; accepted to A&A
- Published
- 2017
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