The description of stellar interior remains as a big challenge for the
nuclear astrophysics community. The consolidated knowledge is restricted to
density regions around the saturation of hadronic matter ρ0=2.8×1014gcm−3, regimes where our nuclear models are successfully
applied. As one moves towards higher densities and extreme conditions up to
five to twenty times ρ0, little can be said about the microphysics of
such objects. Here, we employ a Markov Chain Monte Carlo (MCMC) strategy to
access the variability of polytropic three-pircewised models for neutron star
equation of state. With a fixed description of the hadronic matter, we explore
a variety of models for the high density regimes leading to stellar masses up
to 2.5M⊙. In addition, we also discuss the use of a Bayesian power
regression model with heteroscedastic error. The set of EoS from the Laser
Interferometer Gravitational-Wave Observatory (LIGO) was used as inputs and
treated as data set for testing case.Comment: Minor typo fixes in the title and few typos corrected in the text.
Added funding from Brookhave