Quark formation and phenomenology in binary neutron-star mergers using V-QCD

TL;DR

This study uses advanced simulations with novel equations of state based on V-QCD to explore quark matter formation in neutron-star mergers, revealing multiple post-merger phases and constraining nuclear matter properties through multi-messenger observations.

Contribution

It introduces a new finite-temperature V-QCD framework for neutron-star matter and analyzes quark formation processes in merger simulations, providing insights into the equation of state constraints.

Findings

Identification of three post-merger stages with mixed and pure quark matter.

Collapse due to phase transition occurs within 10 ms post-merger.

The softest equation of state is inconsistent with GW170817's observed lifetime.

Abstract

Using full 3+1 dimensional general-relativistic hydrodynamic simulations of equal- and unequal-mass neutron-star binaries with properties that are consistent with those inferred from the inspiral of GW170817, we perform a detailed study of the quark-formation processes that could take place after merger. We use three equations of state consistent with current pulsar observations derived from a novel finite-temperature framework based on V-QCD, a non-perturbative gauge/gravity model for Quantum Chromodynamics. In this way, we identify three different post-merger stages at which mixed baryonic and quark matter, as well as pure quark matter, are generated. A phase transition triggered collapse already $\lesssim 10\,\rm{ms}$ after the merger reveals that the softest version of our equations of state is actually inconsistent with the expected second-long post-merger lifetime of GW170817. Our results underline the impact that multi-messenger observations of binary neutron-star mergers can have in constraining the equation of state of nuclear matter, especially in its most extreme regimes.