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

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dc.creatorLee, William H.
dc.creatorKluzniak, Wlodzimierz
dc.creatorNix, Jon
dc.date2002-01-08
dc.date.accessioned2026-07-07T02:02:10Z
dc.date.available2026-07-07T02:02:10Z
dc.descriptionWe 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.
dc.descriptionActa Astronomica, in press, 2001
dc.identifierhttps://arxiv.org/abs/astro-ph/0201114
dc.identifierhttp://arxiv.org/abs/astro-ph/0201114
dc.identifierActa Astron. 51 (2001) 331
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3997
dc.subjectAstrophysics
dc.titleBinary coalescence of a strange star with a black hole: Newtonian results
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