  On February 23, 1987 we collected 24 neutrinos from the explosion of a blue
super-giant star in the Large Magellanic Cloud confirming the basic paradigm of
core-collapse supernova. During the many years we have been waiting for a
repeat of that momentous day, the number and size of neutrino detectors around
the world has grown considerably. If the neutrinos from the next supernova in
our Galaxy arrive tomorrow we shall collect upwards of tens of thousands of
events and next generation detectors will increase the amount of data we
collect by more than an order of magnitude. But it is also now apparent that
the message is much more complex than previously thought because many time,
energy and neutrino flavor dependent features are imprinted upon the signal
either 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 at
high temperatures and densities, and the properties of neutrinos. In this
proceedings I will present some aspects of the physics of supernova neutrino
oscillations and what we should expect to observe when the neutrinos from the
next Galactic supernova (eventually) arrive.
