General Relativistic Hydrodynamic Simulations of mergers of strange quark stars
ORAL
Abstract
In this work we perform simulations of mergers of binary strange quark stars in full 3+1 general relativity. For the equilibrium description of strange quark matter, we employ 2 prescriptions of the dense matter equation of state (EoS). Primarily, we describe the cold strange star matter with a Bag-model EoS and approximately include thermal effects by means of an ideal Gamma-law description. Secondarily, we incorporate thermal effects by constructing a full finite-temperature dependent formalism. We contrast the primary observable of gravitational wave strain between the two cases to emphasize the relative influence of thermal effects. We find that the postmerger emission is different between the two treatments however, the characteristic peak frequency in the postmerger is still at par with those observed from mergers of neutron stars. Our study therefore cannot distinguish such mergers from mergers of binary neutron stars.
*We acknowledge funding from the U.S. Department of Energy, Office of Science, Division of Nuclear Physics under Award Number(s) DE-SC0021177 and DE-SC0024388, and from the National Science Foundation under Grants No. PHY-2011725, PHY-2020275, PHY-2116686, AST-2108467, and Award Number 2020275.
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Publication: Phys. Rev. D 111, 083009
Presenters
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Aviral Prakash
- University of California Berkeley