SN 1987A is a unique object and will stay the best observed SN until another galactic SN happens. Not relying on luck, large surveys today provide a rich source of information for SN theory. But they only provide one or a few aspects per SN (e.g. lightcurves, NS/BH masses, ...). Theoretically, a large parameter space (zero-age main-sequence mass, metallicity, multiplicity, ...) needs to be covered to derive a statistical picture analogous to the observational surveys. Stellar evolution, the neutrino-driven explosion mechanism (the most promising and well-explored), and the expansion of the shock wave beyond the star's surface need to be simulated, ideally with a first-principle approach and without symmetry constraints (3D). Due to the comp...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
To place core-collapse supernovae (SNe) in context with the evolution of massive stars, it is necess...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
We present results from a self-consistent, non-rotating core-collapse supernova simulation in three ...
Core-collapse supernovae (SNe) are powerful neutrino sources and as such important targets for the g...
A core-collapse supernova (CCSN) is an astronomical explosion that indicates the death of a massive ...
Core-collapse supernovae (SNe) are the highly energetic explosions of massive stars (≳ 8 M☉) that ar...
A core-collapse supernova (CCSN) is an astronomical explosion that indicates the death of a massive ...
Many young, massive stars are found in close binaries. Using population synthesis simulations. we pr...
Core-collapse supernovae (CCSNe) theories have been long developed to link the observed SNe to their...
A core-collapse supernova (CCSN) is an astronomical explosion that indicates the death of a massive ...
New wide-field and high-cadence transient surveys have enabled us to watch supernovae (SNe) from the...
New wide-field and high-cadence transient surveys have enabled us to watch supernovae (SNe) from the...
Core-collapse supernovae (SNe) are powerful neutrino sources and as such important targets for the g...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
To place core-collapse supernovae (SNe) in context with the evolution of massive stars, it is necess...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
We present results from a self-consistent, non-rotating core-collapse supernova simulation in three ...
Core-collapse supernovae (SNe) are powerful neutrino sources and as such important targets for the g...
A core-collapse supernova (CCSN) is an astronomical explosion that indicates the death of a massive ...
Core-collapse supernovae (SNe) are the highly energetic explosions of massive stars (≳ 8 M☉) that ar...
A core-collapse supernova (CCSN) is an astronomical explosion that indicates the death of a massive ...
Many young, massive stars are found in close binaries. Using population synthesis simulations. we pr...
Core-collapse supernovae (CCSNe) theories have been long developed to link the observed SNe to their...
A core-collapse supernova (CCSN) is an astronomical explosion that indicates the death of a massive ...
New wide-field and high-cadence transient surveys have enabled us to watch supernovae (SNe) from the...
New wide-field and high-cadence transient surveys have enabled us to watch supernovae (SNe) from the...
Core-collapse supernovae (SNe) are powerful neutrino sources and as such important targets for the g...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...
To place core-collapse supernovae (SNe) in context with the evolution of massive stars, it is necess...
Many young, massive stars are found in close binaries. Using population synthesis simulations we pre...