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Strange Star Equations of State Revisited

Published online by Cambridge University Press:  05 March 2013

Debora P. Menezes*
Depto de Física – CFM – CP476, Universidade Federal de Santa Catarina, Florianópolis – SC, Brazil School of Physics, University of Sydney, Sydney NSW 2006, Australia
Don B. Melrose
School of Physics, University of Sydney, Sydney NSW 2006, Australia
CCorresponding author. Email:,
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Motivated by recent suggestions that strange stars can be responsible for glitches and other observational features of pulsars, 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 colour–flavour 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.

Research Article
Copyright © Astronomical Society of Australia 2005


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