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The fine line between total and partial tidal disruption events

Deborah MainettiINAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), ItalyAlessandro LupiInstitut d'Astrophysique de Paris , Sorbonne Universités , UPMC Univ ParisS. CampanaINAF , Osservatorio Astronomico di Brera , via E. Bianchi 46 , 23807 Merate ( LC) , ItalyMonica ColpiINFN , Sezione di Milano-Bicocca , Piazza della Scienza 3 , 20126 Milano , ItalyEric R. CoughlinAstronomy Department and Theoretical Astrophysics Center , University of California , Berkeley , CA 94720 , USAJames GuillochonHarvard-Smithsonian Center for Astrophysics, The Institute for Theory and Computation, 60 Garden Street, Cambridge, MA-02138, USAE. Ramírez-RuizDepartment of Astronomy & Astrophysics , University of California , Santa Cruz , CA -95064 , USA

2017en

ABI

Annotatsiya

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 (rd) 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 rd depends on the simulation technique. We find that the critical distance (or the so-called critical disruption parameter βd) depends only weakly on the adopted simulation method, being βd = 0.92 ± 0.02 for a γ = 5/3 polytrope and βd = 2.01 ± 0.01 for a γ = 4/3 polytrope.

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DOI: 10.1051/0004-6361/201630092/pdf

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