Binary neutron star merger simulations with hot microscopic equations of state
arXiv:2103.02365 · doi:10.1103/PhysRevD.103.083012
Abstract
We perform binary neutron star merger simulations using a newly derived set of finite-temperature equations of state in the Brueckner-Hartree-Fock approach. We point out the important and opposite roles of finite temperature and rotation for stellar stability and systematically investigate the gravitational-wave properties, matter distribution, and ejecta properties in the postmerger phase for the different cases. The validity of several universal relations is also examined and the most suitable EOSs are identified.
Version submitted to PRD
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Cited by in corpus (6)
- Hot neutron stars and their equation of state
- Microscopic nuclear equation of state at finite temperature and stellar stability
- Non-radial oscillations and gravitational wave emission of hybrid neutron stars
- Thermal effects on nuclear matter properties
- Thermal aspects of neutron star mergers
- Light scalars in neutron star mergers