Quantum gravity effects on compact star cores

Peng Wang; Haitang Yang; Xiuming Zhang

doi:10.1016/j.physletb.2012.10.071

paper

Quantum gravity effects on compact star cores

arXiv:1110.5550 · doi:10.1016/j.physletb.2012.10.071

Abstract

Using the Tolman-Oppenheimer-Volkoff equation and the equation of state of zero temperature ultra-relativistic Fermi gas based on generalized uncertainty principle (GUP), the quantum gravitational effects on the cores of compact stars are discussed. Our results show that $2 m (r) / r$ varies with $r$ . Quantum gravity plays an important role in the region $r \sim 1 0^{3} r_{0}$ , where $r_{0} \sim β_{0} l_{p}$ , $l_{p}$ is the Planck length and $β_{0}$ is a dimensionless parameter accounting for quantum gravity effects. Furthermore, near the center of compact stars, we find that the metric components are $g_{tt} \sim r^{4}$ and $g_{r r} = [1 - r^{2} / (6 r_{0}^{2})]^{- 1}$ . All these effects are different from those obtained from classical gravity. These results can be applied to neutron stars or denser ones like quark stars. The observed masses of neutron stars ( $\leq 2 M_{⊙}$ ) indicate that $β_{0}$ can not exceed $1 0^{37}$ , not as good as the upper bound $β_{0} < 1 0^{34}$ from simple electroweak consideration. This means that incorporating either quantum gravity effects or nuclear interactions, one obtains almost the same mass limits of neutron stars.

12 pages, 1 figure, added brief review on compact stars configurations, abstract expanded, references added, typo corrected, published version

Quantum gravity effects on compact star cores

Abstract

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