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Dr. Elke Müller
Dr. Elke Müller
Press Officer AEI Potsdam
Phone:+49 331 567-7303Fax:+49 331 567-7298

The Paper

1.
The LIGO Scientific Collaboration and The Virgo Collaboration
GW170817: Measurements of neutron star radii and equation of state

GW170817 revisited

October 15, 2018

Updated Analysis of GW170817 by the LIGO and Virgo Collaboration places tight constraints on the neutron star equation of state.

Further analysis of the data from the first direct detection of gravitational waves from neutron stars allows more precise determination of neutron star radii and equation of state.

GW170817: Numerical relativity simulation of a binary neutron star merger

Numerical relativity simulation of two inspiraling and merging neutron stars. Higher densities are shown in red, lower densities are shown in pink.

Paper abstract

On August 17, 2017, the LIGO and Virgo observatories made the first direct detection of gravitational waves from the coalescence of a neutron star binary system. The detection of this gravitational wave signal, GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars.

Our analysis employs two methods: the use of equation-of-state-insensitive relations between various macroscopic properties of the neutron stars and the use of an efficient parameterization of the defining function p(ρ) of the equation of state itself. From the LIGO and Virgo data alone and the first method, we measure the two neutron star radii as R1 = 10.8+2.0/-1.7 km for the heavier star and R2 = 10.7+2.1/-1.5 km for the lighter star at the 90% credible level. If we additionally require that the equation of state supports neutron stars with masses larger than 1.97 M as required from electromagnetic observations and employ the equation of state parametrization, we further constrain R1 = 11.9+1.4/-1.4 km and R2 = 11.9+1.4/-1.4 km at the 90% credible level. Finally, we obtain constraints on p(ρ) at supranuclear densities, with pressure at twice nuclear saturation density measured at 3.5+2.7/-1.7 × 1034 dyn cm−2 at the 90% level.

 
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