  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 $\rho _{0} = 2.8\times
10^{14} {\rm\ g\ cm^{-3}}$, regimes where our nuclear models are successfully
applied. As one moves towards higher densities and extreme conditions up to
five to twenty times $\rho_{0}$, 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 $2.5\ M_{\odot}$. 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.
