Future galactic supernova neutrino signal: What can we learn?

Abstract

The next supernova in our galaxy will be detected by a variety of neutrino detectors. In this lecture I discuss the set of observables needed to constrain the models of supernova neutrino emission. They are the flux normalizations, and average energies, of each of the three expected components of the neutrino flux: ${\nu }_e$, ${\bar{\nu }}_e$, and ${\nu }_x$ (all the other four flavors combined). I show how the existing, or soon to be operational, neutrino detectors will be able to determine the magnitude of these observables, and estimate the corresponding rates.

10 pages, 5 figures, Talk at the School `Neutrinos in Astro, Particle and Nuclear Physics', Erice, September 18-26, 2001

Cited by in corpus (13)

• Detection of Supernova Neutrinos by Neutrino-Proton Elastic Scattering
• Probing supernova shock waves and neutrino flavor transitions in next-generation water-Cherenkov detectors
• Three-generation flavor transitions and decays of supernova relic neutrinos
• What Can Be Learned with a Lead-Based Supernova-Neutrino Detector?
• A Generic Test of Modified Gravity Models which Emulate Dark Matter
• Gravity Gets There First with Dark Matter Emulators
• Reconstructing supernova-neutrino spectra using low-energy beta-beams
• Potential for Supernova Neutrino Detection in MiniBooNE
• Physics with Supernovae
• Supernova Neutrinos: The Accretion Disk Scenario
• Supernova Neutrinos and the LSND Evidence for Neutrino Oscillations
• Effects of degenerate sterile neutrinos on the supernova neutrino flux
• Supernova Neutrinos, LSND and MiniBooNE