Abstract
The structure of light quark star is studied within a new two-flavor NJL model. By retaining the contribution from the vector term in the Fierz-transformed Lagrangian, a two-solar-mass pure quark star is achieved. To overcome the disadvantage of three-momentum truncation in the regularisation procedure, we introduce the proper-time regularisation. We also employ the newly proposed definition of vacuum pressure, in which the quasi-Wigner vacuum (corresponding to the quasi-Winger solution of the gap equation) is used as the reference ground state. Free parameter includes only a mixing constant $\alpha$ which weighs contribution from Fierz-transformed Lagrangian. We constrain $\alpha$ to be around $0.9$ by the observed mass of pulsars $PSR J0348+0432$ and $PSR J1614-2230$. We find the calculated surface energy density meets the requirement ($> 2.80\times10^{14}$g/cm$^3 $). Besides, for a 1.4 solar mass star, the tidal Love number $k_2$ and deformability $\Lambda$ are calculated which satisfies the constrain $200 < \Lambda < 800$.
Highlights
Investigations of dense matter are an important part of studying strong interactions
We find that the calculated surface energy density meets the requirement (>2.80 × 1014 g=cm3) [Phys
For a 1.4-solar-mass star, the deformability Λ is calculated, which is consistent with a recent analysis on the binary neutron star merger GW170817 with Λ in (0,630) for large component spins and 300þ−243200 when restricting the magnitude of the component spins [Phys
Summary
Investigations of dense matter are an important part of studying strong interactions. [20], the parameter α used to reflect the weight of different interaction channels cannot be given in advance by the mean-field theory It must be determined by related experimental data of high-density strong interacting matter. The bag constant B gives the pressure of quark matter at a zero temperature and zero density It is treated as a phenomenological parameter and determined by experimental requirements [21,22,23,24,25,26]. We use a recently proposed definition B 1⁄4 ΩðMWignerÞ − ΩðMNambuÞ [26,30,31], i.e., to subtract from the thermodynamic potential corresponding to the Wigner-Weyl solution Such a definition is more theoretically self-consistent, since the Wigner-Weyl solution is another ( unphysical) solution to the quark gap equation in the NJL model.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
