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

TL;DR

This paper uses Newtonian hydrodynamical simulations to study the merger of quark stars with black holes, revealing that most quark matter is accreted with minimal mass ejection, and a small remnant survives in orbit.

Contribution

It provides the first Newtonian simulation results of quark star-black hole mergers, detailing mass accretion and remnant formation.

Findings

Quark star is disrupted and forms transient accretion structures.

Approximately 0.03 of the original mass remains as a remnant.

Nearly all quark matter is accreted with negligible ejection.

Abstract

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.