AI Article Synopsis
- This study investigates binary-neutron-star (BNS) mergers using quark-hadron crossover (QHC) equations of state (EOS), revealing how these models impact gravitational wave (GW) signals differently from those using purely hadronic matter or traditional phase transitions.
- The findings indicate that for lower-mass binaries, the unique stiffening behavior of QHC models results in lower frequencies of postmerger GW signals compared to hadronic EOS.
- For higher-mass binaries, the behavior of GW frequencies depends on the sound-speed peak found in QHC models, offering insights into quark dynamics at high densities and informing future observations with advanced gravitational wave detectors.
Article Abstract
Fully general-relativistic binary-neutron-star (BNS) merger simulations with quark-hadron crossover (QHC) equations of state (EOS) are studied for the first time. In contrast to EOS with purely hadronic matter or with a first-order quark-hadron phase transition (1PT), in the transition region QHC EOS show a peak in sound speed and thus a stiffening. We study the effects of such stiffening in the merger and postmerger gravitational (GW) signals. Through simulations in the binary-mass range 2.5
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http://dx.doi.org/10.1103/PhysRevLett.129.181101 DOI Listing Publication Analysis
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