QCD Phase Transitions in Binary Neutron Star Mergers: Signatures from multi-modal GW Spectroscopy
ORAL
Abstract
We report on multi-modal gravitational wave (GW) signatures of high-density phase transition to deconfined quarks in the context of binary neutron star (BNS) mergers. We employ state-of-the-art, general relativistic hydrodynamics simulations of BNS mergers in quasi-circular and nearly parabolic orbits and consider equations of state that model different treatments to both hadronic and quark matter. We find that such phase transitions robustly act to suppress the one-armed spiral instability in the postmerger remnant and lead to an anti-correlation between the energy carried by the l=2, m=1 GW mode and the energy density gap between the hadronic and quark phase. Consequently, this manifests as a reduced signal-to-noise ratio for the l=2, m=1 mode in the quark case and whose detection could potentially constrain the energy density gap between the phases.
*Numerical Relativity simulations were performed on Bridges2 and Expanse (NSF XSEDE allocation TG-PHY160025). This research also uses resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DEAC02-05CH11231. We acknowledge support from U.S. Department of Energy, Office of Science, Division of Nuclear Physics under Award No. DE-SC0021177 and the National Science Foundation under Grant No. PHY-2011725, PHY-2116686, PHY-2020275, AST-2108467.
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Presenters
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Aviral Prakash
- The Pennsylvania State University