Speaker
Description
We show how to coherently combine information from a population of sub-threshold, gravitational-wave binary neutron star post-merger remnants to constrain the hot nuclear equation of state. Although no individual event in our synthetic population can be claimed as a confident detection, we show how to statistically determine the fraction of merger events that promptly collapse to form a black hole, compared to those for which a neutron star survives the merger for at least tens of milliseconds. This fraction, when combined with information about the neutron star mass distribution gleaned from the inspiral portion of the signals, provides an indirect measure of the neutron star maximum mass. Using conservative measures of the post-merger waveforms, we show that 50-70 events with binary neutron star inspiral measurements can be combined to give an 11−20% fractional uncertainty on the maximum mass of rapidly rotating, hot neutron stars, which can potentially be turned into a 12−21% fractional constraint on the Tolman-Oppenheimer-Volkoff mass. This measure of the hot nuclear equation of state can be combined with information of cold neutron stars to see the effect of temperature on physics in the densest regions of the Universe.
| Research Area | Gravitational waves: neutron stars and supernovae |
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