Open AccessTidal forces near a black hole with scalar hairy
Author(s) -
Eduardo L. André,
Ivan M. Potashov,
Ju V Tchemarina,
A. N. Tsirulev
Publication year - 2020
Publication title -
journal of physics. conference series
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.21
H-Index - 85
eISSN - 1742-6596
pISSN - 1742-6588
DOI - 10.1088/1742-6596/1690/1/012181
Subject(s) - physics , schwarzschild radius , supermassive black hole , black hole (networking) , event horizon , scalar field , photon sphere , circular orbit , stellar black hole , astrophysics , tidal force , white hole , intermediate mass black hole , rotating black hole , charged black hole , radius , classical mechanics , galaxy , gravitational collapse , event (particle physics) , accretion (finance) , computer network , routing protocol , routing (electronic design automation) , computer security , computer science , link state routing protocol
We deal with static, asymptotically flat, spherically symmetric black holes supported by a minimally coupled scalar field with an arbitrary self-interaction potential. We consider a scalar black hole as a simple model of supermassive black holes in the centers of galaxies surrounded by dark matter. Both the radius of the innermost stable circular orbit and the event horizon radius of such an object are less than those of a Schwarzschild black hole with the same mass. Moreover, they can be arbitrary small, so that tidal forces, acting on a star orbiting a scalar field black hole near its photon sphere, can be extremely large and can disrupt the star. This means, in turn, that tidal effects can play an important role for the interpretation of observations in galactic astrophysics.