Adding rho and phi vector mesons to the vector MIT bag model is claimed to stiffen the strange quark star equation of state and raise the maximum mass to about 2.5 solar masses, but the energy-density formula misses a required interaction term.
On the stability of two-flavor and three-flavor quark stars
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abstract
Following our recenty proposed self-consistent mean-field approximation approach, we have done some researches on the chiral phase transition of strong interaction matter within the framework of Nambu-Jona-Lasinio (NJL) model. The chiral susceptibility and equation of state (EOS) are computed in this work for both two-flavor and three-flavor quark matter for contrast. The Pauli-Villars scheme, which can preserve gauge invariance, is used in this paper. Moreover, whether the three-flavor quark matter is more stable than the two-flavor quark matter or not in quark stars is discussed in this work. In our model, when the bag constant are the same, the two-flavor quark matter has a higher pressure than the three-flavor quark matter, which is different from what Witten proposed in his pioneering work.
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Strange quark stars in modified vector MIT bag model: role of $\rho$ and $\phi$ mesons
Adding rho and phi vector mesons to the vector MIT bag model is claimed to stiffen the strange quark star equation of state and raise the maximum mass to about 2.5 solar masses, but the energy-density formula misses a required interaction term.