  Classical novae are expected to emit gamma rays during their explosions. The
most important contribution to the early gamma-ray emission comes from the
annihilation with electrons of the positrons generated by the decay of 13N and
18F. The photons are expected to be down-scattered to a few tens of keV, and
the emission is predicted to occur some days before the visual discovery and to
last ~2 days. Despite a number of attempts, no positive detections of such
emission have been made, due to lack of sensitivity and of sky coverage.
Because of its huge field of view, good sensitivity, and well-adapted energy
band, Swift/BAT offers a new opportunity for such searches. BAT data can be
retrospectively used to search for prompt gamma-ray emission from the direction
of novae after their optical discovery. We have estimated the expected success
rate for the detection with BAT of gamma rays from classical novae using a
Monte Carlo approach. Searches were performed for emission from novae occurring
since the launch of Swift. Using the actual observing program during the first
2.3 years of BAT operations as an example, and sensitivity achieved, we
estimate the expected rate of detection of classical novae with BAT as
~0.2-0.5/yr, implying that several should be seen within a 10 yr mission. The
search for emission in the directions of the 24 classical novae discovered
since the Swift launch yielded no positive results, but none of these was known
to be close enough for this to be a surprise. Detections of a recurrent nova
(RS Oph) and a nearby dwarf nova (V455 And) demonstrate the efficacy of the
technique. The absence of detections is consistent with the expectations from
the Monte Carlo simulations, but the long-term prospects are encouraging given
an anticipated Swift operating lifetime of ~10 years.
