Equation of state of neutron star matter, limiting rotational periods of fast pulsars, and the properties of strange stars

Details Equation of state of neutron star matter, limiting rotational periods of fast pulsars, and the properties of strange stars Equation of state of neutron star matter, limiting rotational periods of fast pulsars, and the properties of strange stars

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hdnm.procq....w&link_type=abstract

Presented at the NATO Advanced Study Institute on Hot and Dense Nuclear Matter, Bodrum, Turkey, 26 Sept. - 9 Oct. 1993

Physics

Equations Of State, Matter (Physics), Neutron Stars, Pulsars, Stellar Models, Stellar Rotation, Strangeness, Baryons, Nucleons, Quarks, Rotary Stability, Stellar Mass

Scientific paper

The present status of dense nuclear matter calculations and constraints on the behavior of the associated equation of state at high densities from data on rapidly rotating pulsars is reviewed. Recent finding of the likely existence of a mixed phase of baryons and quarks forming a coulomb lattice in the dense cores of neutron stars is discussed. A review of important findings of recently performed calculations of rapidly rotating compact stars is given. These are constructed in the framework of general relativity theory for a representative collection of realistic nuclear equations of state. The minimum possible rotational periods of gravitationally bound neutron stars and self-bound strange stars are established. Its knowledge is of fundamental importance for the decision between pulsars that can be understood as rotating neutron stars and those that cannot (signature of hypothetical self-bound matter of which strange stars are the likely stellar candidates). The properties of sequences of strange stars are investigated. Specifically, the question of whether such objects can give rise to the observed phenomena of pulsar glitches is answered, which is at the present time the only astrophysical test of the strange quark matter hypothesis.

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