The Critical Neutrino Luminosity in Rotating Core-Collapse Supernovae

Details The Critical Neutrino Luminosity in Rotating Core-Collapse Supernovae The Critical Neutrino Luminosity in Rotating Core-Collapse Supernovae

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21943608c&link_type=abstract

American Astronomical Society, AAS Meeting #219, #436.08

Astronomy and Astrophysics

Astronomy

Scientific paper

Numerical simulations of core-collapse supernovae suggest that the critical neutrino luminosity necessary to cause explosions is dependent on dimensionality. The lower threshold for explosion in 2D versus 1D has been well-documented, but recently Nordhaus et al. (2010) have found that going to 3D simulations further reduces the critical neutrino luminosity by around 20 \% as compared with 2D simulations. This result may reflect the fundamental difference in the development of turbulence between 2D and 3D simulations and may indicate that 3D simulations are critically necessary to study core-collapse supernovae. The conclusion that the critical neutrino luminosity is reduced in 3D simulations is not yet well-established, however. Hanke et al. (2011) conducted a study similar to that of Nordhaus et al. and find that, while the critical luminosity in 2D is lower than in 1D, going to 3D does not result in a significantly lowered critical neutrino luminosity for explosion. This leaves open the question of the importance of 3D simulations and what physical mechanisms reduce the critical neutrino luminosity in simulations of core-collapse supernovae. I will discuss our recent effort to examine the dependence of the critical neutrino luminosity on dimensionality. Our approach is similar to those of Nordhaus et al. and Hanke et al., implemented in the FLASH code. We examine the dependence of our results on the equation of state used. We also study the influence of rotation on the critical luminosity. Rotation provides additional large-scale, non-radial motion of the sort Hanke et al. suggest is critical to increasing dwell times in the gain region and, hence, increasing the neutrino heating efficiency.

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