تقرير
Core-collapse supernova explosions triggered by a quark-hadron phase transition during the early post-bounce phase
| العنوان: | Core-collapse supernova explosions triggered by a quark-hadron phase transition during the early post-bounce phase |
|---|---|
| المؤلفون: | Fischer, T., Sagert, I., Pagliara, G., Hempel, M., Schaffner-Bielich, J., Rauscher, T., Thielemann, F. -K., Käppeli, R., Martínez-Pinedo, G., Liebendörfer, M. |
| سنة النشر: | 2010 |
| المجموعة: | Astrophysics High Energy Physics - Phenomenology |
| مصطلحات موضوعية: | Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology |
| الوصف: | 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. The collapse halts in the pure quark phase, where the adiabatic index increases. A strong accretion shock forms, which propagates towards the protoneutron star 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 protoneutron star where the vp-process might occur. Comment: 29 pages, 24 figures, submitted to ApJ |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.1088/0067-0049/194/2/39 |
| URL الوصول: | http://arxiv.org/abs/1011.3409 |
| رقم الأكسشن: | edsarx.1011.3409 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.1088/0067-0049/194/2/39 |
|---|