Even though theoreticians agree that supernova explosions derive their energy from the collapse of the progenitor star's core, they have found it very difficult to confirm this theory numerically. Recently, J. Wilson has succeeded in modelling SN ejection by the "delayed supernova explosion mechanism." According to this mechanism, energy from the progenitor star's core collapse is transferred to the envelope by neutrinos in a delayed fashion. The Principal Investigator (PI) proposes to investigate the viability and necessary conditions of Wilson's mechanism. The PI will use a one-dimensional relativistic hydrodynamic computer code, originally developed by Myra et al. The PI's specific focus will be on how the explosion, the resulting neutron star, and the neutrino emission spectrum are dependent upon the progenitor star's mass and structure. Furthermore, he will calculate theoretical neutrino burst signatures, simulate the star's mantle convection two- dimensionally, and investigate the evolution of X-ray and gamma- ray emissions. The 2-D code has been developed, debugged, and tested by Fryxell. As a final topic, unrelated to SN, the PI proposes to continue with his evolutionary calculations of brown dwarfs and very low mass stars.
