Hybrid Stars

Journal Article · Thu Dec 02 04:00:00 EST 2004 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.1843634· OSTI ID:20630369

Menezes, D P ^[1]; Providencia, C ^[2]

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1. Dep. de Fisica - CFM - Universidade Federal de Santa Catarina - Florianopolis - SC - CP. 476 - CEP 88.040 - 900 (Brazil)
2. Centro de Fisica Teorica - Dep. de Fisica - Universidade de Coimbra - P-3004 - 516 Coimbra (Portugal)

In the present paper we calculate the properties of hybrid stars, namely, its gravitational, baryonic masses and central energy densities by solving the Tolman-Volkoff-Oppenheimer equations, which were derived from Einstein's equations for compact stellar objects. In order to obtain these properties, an adequate equation of state (EOS) is necessary. Hybrid stars are formed when a phase transition to a deconfined phase is thermodinamically possible. In this work we have used the non-linear Walecka model for the hadron matter and the MIT Bag (unpaired quark phase) and the Nambu-Jona-Lasinio (NJL) models for the quark matter in order to build the appropriate equations of state for the mixed phase constituted by hadrons and quarks in {beta}-equilibrium.

• OSTI ID: 20630369
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 739; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
BAG MODEL
BARYONS
BINARY STARS
EINSTEIN FIELD EQUATIONS
ENERGY DENSITY
EQUATIONS OF STATE
EQUILIBRIUM
GRAVITATIONAL WAVES
NONLINEAR PROBLEMS
PHASE TRANSFORMATIONS
QUARK MATTER
QUARKS
WALECKA MODEL