Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
Feb, 2006
15 pages
Published in:
- Phys.Rev.C 74 (2006) 035802
e-Print:
- nucl-th/0602038 [nucl-th]
Report number:
- MPG-VT-UR-270-06
Citations per year
Abstract:
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 , 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.- 97.60.Jd
- 26.60.+c
- 04.40.Dg
- 12.38.Mh
- neutron star
- pulsar: mass
- Urca process
- equation of state: constraint
- nuclear matter: density
- critical phenomena
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