  The recurrent nova RS Oph experienced an outburst in 2006, 21 years after its
previous explosion in 1985, as expected. It was observed at almost all
wavelengths, and important information about its properties is still being
extracted. We present theoretical models of the explosion of this fascinating
object, which indicate that the mass of the accreting white dwarf should be
very close to the Chandrasekhar mass, to allow for such a short recurrence
period. In addition, since models suggest that this nova ejects less mass than
it accretes, it is an excellent candidate for a thermonuclear supernova
explosion, in about $10^5-10^7$ years from now. We also analyze the emission of
soft gamma-rays by RS Oph detected with the BAT instrument onboard Swift, and
with the PCA onboard RXTE. We rule out that this emission has its origin in
radioactive decays in the expanding nova envelope.
