Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions

Details Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions

2006-02-13

arxiv.org/abs/nucl-th/0602038v1

Phys.Rev.C74:035802,2006

Physics

Nuclear Physics

Nuclear Theory

15 pages, 8 figures, 5 tables

Scientific paper

10.1103/PhysRevC.74.035802

A new scheme for testing nuclear matter equations of state (EsoS) at high densities using constraints from neutron star phenomenology and a flow data analysis of heavy-ion collisions is suggested. An acceptable EoS shall not allow the direct Urca process to occur in neutron stars with masses below $1.5~M_{\odot}$, and also shall not contradict flow and kaon production data of heavy-ion collisions. Compact star constraints include the mass measurements of 2.1 +/- 0.2 M_sun (1 sigma level) for PSR J0751+1807, of 2.0 +/- 0.1 M_sun from the innermost stable circular orbit for 4U 1636-536, the baryon mass - gravitational mass relationships from Pulsar B in J0737-3039 and the mass-radius relationships from quasiperiodic brightness oscillations in 4U 0614+09 and from the thermal emission of RX J1856-3754. This scheme is applied to a set of relativistic EsoS constrained otherwise from nuclear matter saturation properties with the result that no EoS can satisfy all constraints simultaneously, but those with density-dependent masses and coupling constants appear most promising.

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