Abstract
Quark matter with only and quarks () might be the ground state of baryonic matter at large baryon number . With , this has no direct conflict with the stability of ordinary nuclei. An intriguing test of this scenario is to look for quantum nucleation of inside neutron stars due to their large baryon densities. In this paper, we study the transition rate of cold neutron stars to quark stars () and the astrophysical implications, considering the relevant theoretical uncertainties and observational constraints. It turns out that a large portion of parameter space predicts an instantaneous transition, and so the observed neutron stars are mostly . We find this possibility still viable under the recent gravitational wave and pulsar observations, although there are debates on its compatibility with some observations that involve some complex structures of quark matter. The tension could be partially relieved in the two-families scenario, where the high-mass stars () are all and the low-mass ones () are mostly hadronic stars. In this case, the slow transition of the low-mass hadronic stars points to a very specific class of hadronic models with moderately stiff EOSs, and properties are also strongly constrained.
4 More- Received 30 June 2020
- Accepted 15 September 2020
DOI:https://doi.org/10.1103/PhysRevD.102.083003
Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Funded by SCOAP3.
Published by the American Physical Society