Core-Collapse Supernovae and Other Outcomes of Stellar Collapse
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)