https://doi.org/10.1140/epja/i2006-08-044-3
Nuclear Physics in Astrophysics II
Equation of state of strongly interacting matter in compact stars
1
Dipartimento di Fisica, Politecnico di Torino, 10129, Torino, Italy
2
Sezione di Torino, INFN, 10125, Torino, Italy
3
Sezione di Ferrara, INFN, 44100, Ferrara, Italy
* e-mail: pagliara@fe.infn.it
Received:
17
June
2005
Accepted:
20
December
2005
Published online:
21
March
2006
We study the equation of state of strongly interacting matter at large densities and vanishing temperature. The hadronic matter equation of state is computed in a relativistic mean-field model and the quark matter equation of state is computed using a NJL-type model which takes into account the possibility of formation of the gapless color flavor locked phase. We focus in particular on the possible phase transition from hadronic matter to quark matter using both Maxwell and Gibbs constructions. We finally discuss the relevance of the equation of state in the context of compact stars and we propose some astrophysical signatures of the presence of quark matter in compact stars.
PACS: 26.60.+c Nuclear matter aspects of neutron stars – / 25.75.Nq Quark deconfinement, quark-gluon plasma production, and phase transitions –
© Società Italiana di Fisica and Springer-Verlag, 2006
