Model Study of a Quark Star

Abstract

In this paper we apply the equation of state (EOS) of QCD at finite chemical potential and zero temperature proposed in H. S. Zong and W. M. Sun [Int. J. Mod. Phys. {\bf A23}, 3591 (2008)] to the study of properties of quark star. This EOS contains only one adjustable parameter $m_D$ which sets the scale of chiral symmetry breaking (in our calculation we have chosen two values of $m_D$: $m_D=244MeV$ and $m_D=239MeV$, which is fitted from the value of $f_{\pi }$ and determined by $e^{+}{e}^{-}$ annihilation experiment, respectively). From this EOS a model of quark star is established by applying the Tolman-Oppenheimer-Volkoff equation under two conditions: with the $P(\mu =0)$ term and without the $P(\mu =0)$ term. Our results show clearly that the $P(\mu =0)$ term is an important quantity in the study of quark star. A comparison between our model and other models of quark star is made. In particular, we have compared our results with the most recent observational data measured using Shapiro delay reported in P.B. Demorest et al. [Nature (London) {\bf 467}, 1081 (2010)].

14 pages, 6 figures, 1 table

References in corpus (4)

• Shapiro delay measurement of a two solar mass neutron star
• Quark matter in compact stars?
• The calculation of the equation of state of QCD at finite chemical potential and zero temperature
• The thermal evolution of nuclear matter at zero temperature and definite baryon number density in chiral perturbation theory

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• Connecting neutron star observations to the high density equation of state of quasi-particle model
• Kaon meson condensate in neutron star matter including hyperons
• Self-bound Interacting QCD Matter in Compact Stars
• The existence of a two-solar mass neutron star constrains the gravitational constant G_N at strong field
• Calculation of bulk viscosity of QCD at zero temperature and finite chemical potential
• Kaon-meson coupling from SU(3) flavour symmetry and application to antikaon condensed dense matter in neutron star