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Quark phases in neutron stars and a "third family" of compact stars as a signature for phase transitions
The appearance of quark phases in the dense interior of neutron stars provides one possibility to soften the equation of state (EOS) of neutron star matter at high densities. This softening leads to more compact equilibrium configurations of neutron stars compared to pure hadronic stars of the same...
| Autores principales: | , , , |
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| Lenguaje: | eng |
| Publicado: |
2000
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| Materias: | |
| Acceso en línea: | https://dx.doi.org/10.1016/S0375-9474(00)00305-5 http://cds.cern.ch/record/424364 |