Neutron and quark stars: constraining the parameters for simple EoS using the GW170817
Abstract
It is well known that the equation of state (EoS) of compact objects like neutron and quark stars is not determined despite there are several sophisticated models to describe it. From the electromagnetic observations, summarized in Lattimer and Prakash (2001), and the recent observation of gravitational waves from binary neutron star inspiral GW170817 Abbott et al. (2017) and GW190425 The LIGO Scientific Collaboration et al. (2020), it is possible to make an estimation of the range of masses and so constraint the mass of the neutron and quark stars, determining not only the best approximation for the EoS, but which kind of stars we would be observing. In this paper we explore several configurations of neutron stars assuming a simple polytropic equation of state, using a single layer model without crust. In particular, when the EoS depends on the mass rest density, p =K ρ_{0}^{Γ}, and when it depends on the energy density p =K ρ^{Γ}, considerable differences in the massradius relationships are found. On the other hand, we also explore quark stars models using the MIT bag EoS for different values of the vacuum energy density B.
 Publication:

Astrophysics and Space Science
 Pub Date:
 February 2020
 DOI:
 10.1007/s1050902003756y
 arXiv:
 arXiv:2002.08879
 Bibcode:
 2020Ap&SS.365...43A
 Keywords:

 Neutron and quark stars;
 Relativistic atrophysics;
 Equation of state;
 General Relativity and Quantum Cosmology;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 7 pages, 4 figures and 1 table