Strange star equations of state revisited
arXiv:astro-ph/0506158 · doi:10.1071/AS05022
Abstract
Motivated by recent suggestions that strange stars can be responsible for glitches and other observational features of pulsar, we review some possible equations of state and their implications for models of neutron, hybrid and strange stars. We consider the MIT bag model and also strange matter in the color-flavored-locked phase. The central energy densities for strange stars are higher than the central densities of ordinary neutron stars. Strange stars are bound by the strong force and so can also rotate much faster than neutron stars. These results are only weakly dependent on the model used for the quark matter. If just one of the existing mass to radius ratio constraint is valid, most neutron stars equations of state are ruled out, but all the strange stars equations of state presented in this work remain consistent with the constraint.
arXiv comment9 pages, 5 figures, 2 tables
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Cited by in corpus (7)
- Quark stars within relativistic models
- Quark matter equation of state and stellar properties
- The importance of the mixed phase in hybrid stars built with the Nambu-Jona-Lasinio model
- Density Dependent Parametrization Models: Formalism and Applications
- How Neutron Star Observations Point Towards Exotic Matter: Existing Explanations and a Prospective Proposal
- Electrically charged pulsars
- The compressibility of quark matter under strong magnetic field in the NJL model