Nuclear Matter Equations of State and the Neutron Stars

Journal Article · Mon May 12 04:00:00 EDT 2008 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.2939317· OSTI ID:21143367

Urbanec, M; Stuchlik, Z ^[1]; Betak, E ^[1]

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1. Institute of Physics, Fac. of Philos. and Sci., Silesian Univ., 74601 Opava (Czech Republic)

The equations of state (EoS) of relativistic asymmetric nuclear matter are obtainable from assumed form of the interaction Lagrangian. They are one of important inputs to describe the neutron stars. The structure of the neutron stars, i.e. the density of matter and the pressure as functions of radial distance starting from their values at the center of a star, is straightforwardly dependent on EoS. Similarly, a limitation on the total mass of the neutron star can be obtained therefrom. Thus, EoS and the underlying nucleon interactions can be tested also by the means of astronomical observations.

• OSTI ID: 21143367
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 1012; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
ASYMMETRY
EQUATIONS OF STATE
LAGRANGIAN FUNCTION
NEUTRON DENSITY
NEUTRON STARS
NUCLEAR MATTER
NUCLEAR STRUCTURE
NUCLEON-NUCLEON INTERACTIONS
NUCLEONS
RELATIVISTIC RANGE
THERMODYNAMICS