Constraining the neutron star equation of state using multi-band independent measurements of radii and tidal deformabilities. (arXiv:1902.05078v1 [astro-ph.HE])

<a href="http://arxiv.org/find/astro-ph/1/au:+Fasano_M/0/1/0/all/0/1">Margherita Fasano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abdelsalhin_T/0/1/0/all/0/1">Tiziano Abdelsalhin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maselli_A/0/1/0/all/0/1">Andrea Maselli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrari_V/0/1/0/all/0/1">Valeria Ferrari</a>

Using a Bayesian approach, we combine measurements of neutron star

macroscopic observables obtained by astrophysical and gravitational

observations, to derive joint constraints on the equation of state (EoS) of

matter at supranuclear density. In our analysis we use two sets of data: (i)

the masses and tidal deformabilities measured in the binary neutron star event

GW170817, detected by LIGO and Virgo; (ii) the masses and stellar radii

measured from observations of nuclear bursts in accreting low-mass X-ray

binaries. Using two different parametrizations of the equation of state, we

compute the posteriorprobability distributions of the EoS parameters, using

which we infer the posterior distribution for the radius and the mass of the

two neutron stars of GW170817. The constraints we set on the radii are tighter

than previous bounds.

Using a Bayesian approach, we combine measurements of neutron star

macroscopic observables obtained by astrophysical and gravitational

observations, to derive joint constraints on the equation of state (EoS) of

matter at supranuclear density. In our analysis we use two sets of data: (i)

the masses and tidal deformabilities measured in the binary neutron star event

GW170817, detected by LIGO and Virgo; (ii) the masses and stellar radii

measured from observations of nuclear bursts in accreting low-mass X-ray

binaries. Using two different parametrizations of the equation of state, we

compute the posteriorprobability distributions of the EoS parameters, using

which we infer the posterior distribution for the radius and the mass of the

two neutron stars of GW170817. The constraints we set on the radii are tighter

than previous bounds.

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