  Microquasar SS433 is composed by a supergiant star that feeds mass through a
supercritical accretion disk to a $\sim 10 \ M_\odot$ black hole. The latter
launches two oppositely directed jets that precess with a period of $162$ days.
The system has been detected at different spatial scales in frequencies ranging
from radio to gamma rays, and has long been considered as a potential neutrino
source which has been observed by AMANDA in the past, and later IceCube,
leading to more restrictive upper bounds on the neutrino flux. In this work, we
explore the possibilities that neutrinos could be produced in the jets of this
source at levels consistent, or at least, not incompatible with any current
data on electromagnetic emission available. In order to do so, we consider the
injection of both electrons and protons at different positions in the jets, and
we compute their broadband photon emission by synchrotron and interactions with
ambient photons and matter. After correcting the high energy photon flux by the
effect of $\gamma\gamma$ and $\gamma N$ absorption, we obtain the surviving
flux that arrive on Earth and compare it with observational data by gamma-ray
detectors. The flux of high energy neutrinos is consistently computed and we
find that if they are eventually detected with IceCube, production must take
place at the inner jets, where gamma-ray absorption is important, in order to
avoid current VHE constraints form HESS and MAGIC. {Additionally, we find that
if the flux of 25 TeV gamma-rays recently detected with HAWC and which
corresponds to the jet termination region were produced mainly by $pp$
interactions, this would lead to a too faint neutrino flux that is beyond the
reach of IceCube in its present configuration.
