高能暂现源 · 每日文献综述

Binary neutron star mergers are thought to produce hot, rapidly rotating neutron stars with masses that can far exceed their Tolman─Oppenheimer─Volkoff mass. The gravitational-wave emission from such remnants provides a unique opportunity to measure the nuclear equation of state at densities and temperatures not available to terrestrial experiments. Current detector design is informed by gravitational-wave signals from general relativistic hydrodynamics simulations of neutron star mergers, typically with hybrid thermal treatments for the equation of state, where a cold equation of state is modified by adding a thermal component. We use realistic equations of state based on the relativistic mean field model with consistent treatment of thermal effects to compute the distribution of expected peak gravitational-wave frequencies. Marginalizing over equation of state and progenitor neutron star masses, we show the peak frequency of emission ranges from <inline-formula><tex-math>${\sim} 2.5$</tex-math></inline-formula> to 4 kHz. The width of this distribution suggests the need for broad-band observatories with kHz sensitivity, and calls into question some of the so-called post-merger optimized configurations. We show the proposed KAGRA high-frequency design is well-suited to measuring post-merger remnants when compared to the KAGRA broad-band design.