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On February 23, 1987 we collected 24 neutrinos from the explosion of a bluesuper-giant star in the Large Magellanic Cloud confirming the basic paradigm ofcore-collapse supernova. During the many years we have been waiting for arepeat of that momentous day, the number and size of neutrino detectors aroundthe world has grown considerably. If the neutrinos from the next supernova inour Galaxy arrive tomorrow we shall collect upwards of tens of thousands ofevents and next generation detectors will increase the amount of data wecollect by more than an order of magnitude. But it is also now apparent thatthe message is much more complex than previously thought because many time,energy and neutrino flavor dependent features are imprinted upon the signaleither at emission or by the passage through the outer layers of the star.These features arise due to the explosion dynamics, the physics of nuclei athigh temperatures and densities, and the properties of neutrinos. In thisproceedings I will present some aspects of the physics of supernova neutrinooscillations and what we should expect to observe when the neutrinos from thenext Galactic supernova (eventually) arrive.

The Physics Of Supernova Neutrino Oscillations