Gravitational-wave imprints of non-convex dynamics in binary neutron star mergers
Physical Review D(2024)
摘要
Explaining gravitational-wave (GW) observations of binary neutron star (BNS)
mergers requires an understanding of matter beyond nuclear saturation density.
Our current knowledge of the properties of high-density matter relies on
electromagnetic and GW observations, nuclear physics experiments, and general
relativistic numerical simulations. In this paper we perform
numerical-relativity simulations of BNS mergers subject to non-convex dynamics,
allowing for the appearance of expansive shock waves and compressive
rarefactions. Using a phenomenological non-convex equation of state we identify
observable imprints on the GW spectra of the remnant. In particular, we find
that non-convexity induces a significant shift in the quasi-universal relation
between the peak frequency of the dominant mode and the tidal deformability (of
order Δ f_ peak≳ 380 Hz) with respect to that of
binaries with convex (regular) dynamics. Similar shifts have been reported in
the literature, attributed however to first-order phase transitions from
nuclear/hadronic matter to deconfined quark matter. We argue that the ultimate
origin of the frequency shifts is to be found in the presence of anomalous,
non-convex dynamics in the binary remnant.
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