Bereiche | Tage | Auswahl | Suche | Aktualisierungen | Downloads | Hilfe

HK: Fachverband Physik der Hadronen und Kerne

HK 28: Nuclear Astrophysics II

HK 28.5: Vortrag

Dienstag, 19. März 2019, 17:45–18:00, HS 16

Parametrized Core-Collapse Supernova Simulations in Spherical Symmetry — •Kevin Ebinger¹, Sanjana Curtis², Carla Fröhlich², Matthias Hempel³, Albino Perego⁴, Matthias Liebendörfer³, and Friedrich-Karl Thielemann^1,3 — ¹GSI Helmholtzzentrum für Schwerionenforschung, D-64291 Darmstadt, Germany — ²Department of Physics, North Carolina State University, Raleigh NC 27695 — ³Department für Physik, Universität Basel, CH-4056 Basel, Switzerland — ⁴Istituto Nazionale di Fisica Nucleare, Sezione Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy

Core-collapse supernovae (CCSNe) are explosions of stars that have reached their lives’ end. These extreme events lead to the formation of a neutron star or a black hole and allow for the synthesis of elements heavier than iron that can be ejected and contribute to the galactic chemical evolution. To investigate the complex explosion mechanism of CCSNe, computationally expensive multi-dimensional simulations are required. If one wants to investigate the outcome, global trends and the dependency on the progenitor star for large samples of CCSNe, such multi-dimensional simulations become prohibitively resource consuming. We use a parametrized framework, the PUSH method, to investigate CCSNe for a large sample of progenitor models with solar and lower metallicities. This method allows us to identify trends of CCSNe with progenitor properties, compute nucleosynthesis yields that can be used in galactic chemical evolution models and predict remnant properties that can be compared with observations.