"Binary Neutron Star Mergers in the QCD Phase Diagram" by Matthias Hanauske (Goethe University Frankfurt)
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Europe/Amsterdam
Nikhef
Nikhef
Description
The long-awaited detection of a gravitational wave (GW) from the merger of
a binary neutron star in August 2017 (GW170817) marks the beginning of the
new field of multi-messenger gravitational wave astronomy. Exploiting the
extracted tidal deformations of the two neutron stars from the late
inspiral phase of GW170817 it is now possible to severely constrain
several global properties of the equation of state (EOS) of neutron star
matter. However, the most interesting part of the high density and
temperature regime of the EOS is solely imprinted in the post-merger GW
emission from the remnant hypermassive/supramassive neutron star
(HMNS/SMNS). This regime was not observed in GW170817, but will possibly
be detected in forthcoming events within the next observing run. Based on
a large number of numerical-relativity simulations of merging neutron star
binaries, the emitted GWs, the interior structure of the generated
HMNS/SMNS and the evolution of the underlying matter of the remnant in the
phase diagram of quantum chromodynamics (QCD phase diagram) have been
analyzed in detail. This talk will focus on the consequences of a
potential appearance of a hadron-quark phase transition in the interior
region of the produced HMNS/SMNS and its connection with the spectral
properties of the emitted GW.
