How can we determine luminosities and temperatures of all SNII neutrino flavors

Petr Vogel, Caltech

Abstract:
If r-process occurs in SNII, the neutrino flux, its temperature, and flavor 
composition, are the determining factors. It is crucial for understanding 
the r-process to determine the intensity and temperature of all three 
components (\nu_e, \bar{\nu}_e, \nu_x) of the SN neutrino flux. Detection 
of the \bar{\nu}_e and \nu_e neutrinos through the charged current reaction 
allows one to determine the flux and temperature of these flavors. However, 
the $\nu_x$ neutrinos (mu and tau and their antiparticles) interact only by 
the neutral current reactions, usually with no spectral information. 
We have shown that the neutrino elastic scattering on protons is unique
in that respect, since it can be used for that purpose in a detector with very 
low threshold and background. The KamLAND detector, which just began operation,
has the required properties. I will describe how this task can be accomplished.
Thus, when a next galactic supernova occurs, we will have a rather accurate set
of observations that will form a firm basis for modeling of the r-process.