Neutrino signatures of supernova shock and reverse shock propagation

Details Neutrino signatures of supernova shock and reverse shock propagation Neutrino signatures of supernova shock and reverse shock propagation

2004-07-07

arxiv.org/abs/astro-ph/0407132v2

JCAP 0409 (2004) 015

Astronomy and Astrophysics

Astrophysics

23 pages, 27 eps figures (high resolution plots are available on request), JCAP style; v2: figure 8 extended, matches publishe

Scientific paper

10.1088/1475-7516/2004/09/015

A few seconds after bounce in a core-collapse supernova, the shock wave passes the density region corresponding to resonant neutrino oscillations with the ``atmospheric'' neutrino mass difference. The transient violation of the adiabaticity condition manifests itself in an observable modulation of the neutrino signal from a future galactic supernova. In addition to the shock wave propagation effects that were previously studied, a reverse shock forms when the supersonically expanding neutrino-driven wind collides with the slower earlier supernova ejecta. This implies that for some period the neutrinos pass two subsequent density discontinuities, giving rise to a ``double dip'' feature in the average neutrino energy as a function of time. We study this effect both analytically and numerically and find that it allows one to trace the positions of the forward and reverse shocks. We show that the energy dependent neutrino conversion probabilities allow one to detect oscillations even if the energy spectra of different neutrino flavors are the same as long as the fluxes differ. These features are observable in the \bar\nu_e signal for an inverted and in the \nu_e signal for a normal neutrino mass hierarchy, provided the 13-mixing angle is ``large'' (sin^2\theta_{13}\gg 10^{-5}).

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