Binary coalescence of a strange star with a black hole: Newtonian results

Details Binary coalescence of a strange star with a black hole: Newtonian results Binary coalescence of a strange star with a black hole: Newtonian results

2002-01-08

arxiv.org/abs/astro-ph/0201114v1

Acta Astron. 51 (2001) 331

Astronomy and Astrophysics

Astrophysics

Acta Astronomica, in press, 2001

Scientific paper

We present Newtonian three-dimensional hydrodynamical simulations of the merger of quark stars with black holes. The initial conditions correspond to non-spinning stars in Keplerian orbits, the code includes gravitational radiation reaction in the quadrupole approximation for point masses. We find that the quark star is disrupted, forming transient accretion structures around the black hole, but 0.03 of the original stellar mass survives the initial encounter and remains in an elongated orbit as a rapidly rotating quark starlet, in all cases. No resolvable amount of mass is dynamically ejected during the encounters--the black hole eventually accretes 99.99% +/- 0.01% of the quark matter initially present.

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