Study of rotational quark stars and hybrid stars based on the latest equation of state and observation data

Abstract

In this paper we utilize our improved quasiparticle model to obtain the equation of state (EOS) and use it as an input to the Tolman-Oppenheimer-Volkoff (TOV) equation to get the mass-radii relation of a pure quark star. We discuss the relation between structures of quark stars and the parameters in the EOS and get a maximum mass of quark star over two solar mass. To compare the result with recent observation, we also calculate the structure of a hybrid star and consider the influence of rotation. Finally, the hadron-quark phase transition in the interior of neutron stars and how much energy will be released when a neutron star bursts into a quark star are discussed.