  Nova Mon 2012 is the third gamma-ray transient identified with a
thermonuclear runaway on a white dwarf, that is, a nova event. Swift monitoring
has revealed the distinct evolution of the harder and super-soft X-ray spectral
components, while Swift-UV and V and I-band photometry show a gradual decline
with subtle changes of slope. During the super-soft emission phase, a coherent
7.1 hr modulation was found in the soft X-ray, UV, optical and near-IR data,
varying in phase across all wavebands. Assuming this period to be orbital, the
system has a near-main sequence secondary, with little appreciable stellar
wind. This distinguishes it from the first GeV nova, V407 Cyg, where the
gamma-rays were proposed to form through shock-accelerated particles as the
ejecta interacted with the red giant wind. We favor a model in which the
gamma-rays arise from the shock of the ejecta with material close to the white
dwarf in the orbital plane. This suggests that classical novae may commonly be
GeV sources. We ascribe the orbital modulation to a raised section of an
accretion disk passing through the line of sight, periodically blocking and
reflecting much of the emission. The disk must, therefore, have reformed by day
150 after outburst.
