Evolution of equal mass binary bare quark stars in full general relativity: could a supramassive merger remnant experience prompt collapse?

TL;DR

This study uses full general relativistic simulations to explore the post-merger evolution of equal-mass binary quark stars, identifying the threshold mass for prompt black hole formation and highlighting differences from neutron star mergers.

Contribution

It provides the first detailed analysis of binary quark star mergers in full general relativity, revealing the threshold mass for collapse and its relation to the mass shedding limit.

Findings

Threshold mass for prompt collapse is between 3.05 and 3.10 solar masses.

Threshold mass is close to the mass shedding limit for quark stars.

Binary quark stars with long-lived remnants can collapse to black holes.

Abstract

We have evolved mergers of equal-mass binary quark stars, the total mass of which is close to the mass shedding limit of uniformly rotating configurations, in fully general relativistic hydrodynamic simulations, aimed at investigating the post-merger outcomes. In particular, we have identified the threshold mass for prompt black hole formation after the merger, by tracing the minimum lapse function as well as the amount of ejected material during the merger simulation. A semi-analytical investigation based on the angular momentum contained in the merger remnant is also performed to verify the results. For the equation of state considered in this work, the maximum mass of TOV solutions for which is 2.10 $M_\odot$, the threshold mass is found between 3.05 and 3.10 $M_\odot$. This result is consistent (with a quantitative error smaller than 1%) with the universal relation derived from the numerical results of symmetric binary neutron star mergers. Contrary to the neutron star case, the threshold mass is close to the mass shedding limit of uniformly rotating quark star. Consequently, we have found that binary quark stars with total mass corresponding to the long-lived supramassive remnant for neutron star case, could experience collapse to black hole within several times dynamical timescale, making quark stars as exceptions of the commonly accepted post-merger scenarios for binary neutron star mergers. We have suggested explanation for both the similarity and the difference, between quark stars and neutron stars.