Speed of sound constraints from tidal deformability of neutron stars
A. Kanakis-Pegios, P.S. Koliogiannis, Ch.C. Moustakidis
TL;DR
This paper proposes a method linking tidal deformability measurements of neutron stars to the maximum neutron star mass and the upper bound of the speed of sound in dense matter, using recent gravitational wave observations.
Contribution
It introduces a novel approach to constrain the speed of sound in neutron star matter by relating tidal deformability data to the equation of state stiffness and maximum mass.
Findings
Constraints on the speed of sound from GW170817 and GW190425 data.
Soft equations of state are favored by tidal deformability limits.
Future measurements could tighten bounds on neutron star matter properties.
Abstract
The upper bound of the speed of sound in dense nuclear matter is one of the most interesting but still unsolved problems in Nuclear Physics. Theoretical studies in connection with recent observational data of isolated neutron stars as well as binary neutron stars systems offer an excellent opportunity to shed light on this problem. In the present work, we suggest a method to directly relate the measured tidal deformability (polarizability) of binary neutron stars system (before merger) to the maximum neutron star mass scenario and possible upper bound on the speed of sound. This method is based on the simple but efficient idea that while the upper limit of the effective tidal deformability favors soft equations of state, the recent high measured values of neutron star mass favor stiff ones. In the present work, firstly, using a simple well established model we parametrize the stiffness…
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