  In the framework of the study of the X-ray and optical emission in supernova
remnants we focus on an isolated X-ray knot in the northern rim of the Vela SNR
(Vela FilD), whose X-ray emission has been studied and discussed in Paper I. We
aim at understanding the physical origin of the X-ray and optical emission in
FilD, at understanding the role of the different physical processes at work,
and at obtaining a key for the interpretation of future X-ray observations of
SNRs. To this end we have pursued an accurate ``forward'' modeling of the
interaction of the Vela SNR shock with an ISM cloud. We perform hydrodynamic
simulations and we directly compare the observables synthesized from the
simulations with the data. We explore four different model setups, choosing the
values of the physical parameters on the basis of our preliminary analysis of
the X-ray data. We synthesize X-ray emission maps and spectra filtered through
the XMM-Newton EPIC-MOS instrumental response. The impact of a shock front at 6
million Kelvin on an elliptical cloud 30 times denser than the ambient medium
describes well the shock-cloud interaction processes in the Vela FilD region in
terms of spectral properties and morphology of the X-ray and optical emission.
The bulk of the X-ray emission in the FilD knot originates in the cloud
material heated by the transmitted shock front, but significant X-ray emission
is also associated to the cloud material, which evaporates, as an effect of
thermal conduction, in the intercloud medium. The physical origin of the FilD
optical emission is associated to thermal instabilities. In the FilD knot the
X-ray emission associated to the reflected shock front is negligible.
