Quark cores in extensions of the MIT Bag model

Abstract

Recent observations of massive pulsars having masses of the order of two solar mass pose a new challenge for compact objects such as hybrid stars and neutron stars. Extensions of the bag model and the Nambu-Jona-Lasino model have been used to model these stars to get higher mass stars. Quark matter has been predicted in the cores of these massive stars. In this work we show that an extension of the bag model, with a chemical potential dependent bag parameter can lead to an isentropic phase transition in the core of the neutron star. Our model shows that an EoS having all three quarks $u$, $d$ and $s$ would lead to massive stars with stable quark matter. We find that the mass of the stars not only depends on the bag constant but also on the mass of the strange quark. The mass - radius ratio which determines the redshift values on the surface, indicates that it is possible to obtain stable self bound strange quark matter stars with reasonable values of the bag pressure which correspond to the recent observations of large mass stars.

Significantly revised version, results remain the same

References in corpus (6)

• A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
• Constraining values of bag constant for strange star candidates
• Maximum mass of a hybrid star having a mixed phase region in the light of pulsar PSR J1614-2230
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Cited by in corpus (3)

• Bayesian inference of strange star equation of state using the GW170817 and GW190425 data
• Effects of anisotropic pressure on interacting quark star structure
• Center of mass motion in bag model