Constraining the equation of state of hybrid stars using recent information from multidisciplinary physics

Understand

At the ultra-high densities existing in the core of neutron stars, it is expected that a phase transition from baryonic to deconfined quark matter may occur.

• Such a phase transition would affect the underlying equation of state (EoS) as well as the observable astrophysical properties of neutron stars.
• Comparison of EoS model predictions with astronomical data from multi-messenger signals then provides us an opportunity to probe the behaviour of dense matter.
• In this work, we restrict the allowed parameter space of EoS models in neutron stars for both nucleonic (relativistic mean field model) and quark matter (bag model) sectors by imposing state-of-the-art constraints from nuclear calculations, multi-messenger astrophysical data and perturbative QCD (pQCD).