Core-Collapse Supernovae and Other Outcomes of Stellar Collapse
Christian Ott
Caltech
Core-collapse supernovae from massive stars are among the most energetic
events in the universe. They liberate a mass-energy equivalent of ~15%
of a solar mass in the collapse of their progenitor star's core. The
majority (~99%) of this energy is carried away by neutrinos, while (~1%)
is transferred to the kinetic energy of the explosive outflow. A smaller,
yet still tremendous amount of energy is emitted in electromagnetic and
gravitational waves. I review our current understanding of core collapse
and its range of outcomes. Specifically, I discuss recent insights gained
from new multi-dimensional models on the physical mechanism(s) believed
responsible for converting the gravitational energy liberated in collapse
into energy of the explosion. These models also yield new predictions for
the signature of core-collapse supernovae in neutrinos and gravitational
waves. I outline how their observation from the next nearby core collapse
event can shed light on properties of the progenitor and the dynamics
and thermodynamics of the supernova engine.
Date: | Tuesday, 29 January 2013 |
Time: | 16:00 |
Where: | McGill University |
| Ernest Rutherford Physics Building, R.E. Bell Conference Room (room 103) |
|