  We study the spectral energy distribution of gamma rays and neutrinos in the
precessing microquasar SS433 as a result of pp interactions within its dark
jets. Gamma-ray absorption due to interactions with matter of the extended disk
and of the star is found to be important, as well as absorption caused by the
UV and mid-IR radiation from the equatorial envelopment. We analyze the range
of precessional phases for which this attenuation is at a minimum and the
chances for detection of a gamma-ray signal are enhanced. The power of
relativistic protons in the jets, a free parameter of the model, is constrained
by HEGRA data. This imposes limits on the gamma-ray fluxes to be detected with
instruments such as GLAST, VERITAS and MAGIC II. A future detection of high
energy neutrinos with cubic kilometer telescopes such as IceCube would also
yield important information about acceleration mechanisms that may take place
in the dark jets. Overall, the determination of the ratio of gamma-ray to
neutrino flux will result in a key observational tool to clarify the physics of
heavy jets.
