Abstract
We study the hadron-quark phase transition at finite temperature in the interior of protoneutron stars, combining the Dyson-Schwinger model for quark matter with the Brueckner-Hartree-Fock approach for hadronic matter. We discuss the dependence of the results on different nuclear three-body forces and on details of the quark model. A maximum mass exceeding two solar masses can only be obtained with a strong three-body force and suitable parameter values in the Dyson-Schwinger model. With a hybrid configuration, the maximum mass of protoneutron stars is larger than that of cold neutron stars, such that a delayed collapse might be possible in principle.
- Received 1 March 2012
DOI:https://doi.org/10.1103/PhysRevD.86.045006
© 2012 American Physical Society