• DOI:10.1088/0067-0049/194/2/39
• Corpus ID: 286101

Core-collapse supernova explosions triggered by a quark-hadron phase transition during the early post-bounce phase

@article{Fischer2010CorecollapseSE,
  title={Core-collapse supernova explosions triggered by a quark-hadron phase transition during the early post-bounce phase},
  author={Tobias Fischer and Irina Sagert and G. Pagliara and Matthias Hempel and Jurgen Schaffner-Bielich and Thomas Rauscher and F. Thielemann and Roger Kappeli and Gabriel Mart'inez-Pinedo and Matthias Liebendorfer},
  journal={Astrophysical Journal Supplement Series},
  year={2010},
  volume={194},
  pages={39}
}

• T. Fischer, I. Sagert, +7 authors M. Liebendorfer
• Published 10 November 2010
• Physics
• Astrophysical Journal Supplement Series

We explore explosions of massive stars, which are triggered via the quark-hadron phase transition during the early post-bounce phase of core-collapse supernovae. We construct a quark equation of state, based on the bag model for strange quark matter. The transition between the hadronic and the quark phases is constructed applying Gibbs conditions. The resulting quark-hadron hybrid equations of state are used in core-collapse supernova simulations, based on general relativistic radiation hydrodynamics and three-flavor Boltzmann neutrino transport in spherical symmetry. The formation of a mixed phase reduces the adiabatic index, which induces the gravitational collapse of the central protoneutron star (PNS). The collapse halts in the pure quark phase, where the adiabatic index increases. A strong accretion shock forms, which propagates toward the PNS surface. Due to the density decrease of several orders of magnitude, the accretion shock turns into a dynamic shock with matter outflow. This moment defines the onset of the explosion in supernova models that allow for a quark-hadron phase transition, where otherwise no explosions could be obtained. The shock propagation across the neutrinospheres releases a burst of neutrinos. This serves as a strong observable identification for the structural reconfiguration of the stellar core. The ejected matter expands on a short timescale and remains neutron-rich. These conditions might be suitable for the production of heavy elements via the r-process. The neutron-rich material is followed by proton-rich neutrino-driven ejecta in the later cooling phase of the PNS where the νp-process might occur.