  We present a hadronic model for gamma-ray production in the microquasar LS I
$+61 303$. The system is formed by a neutron star that accretes matter from the
dense and slow equatorial wind of the Be primary star. We calculate the
gamma-ray emission originated in $pp$ interactions between relativistic protons
in the jet and cold protons from the wind. After taking into account opacity
effects on the gamma-rays introduced by the different photons fields, we
present high-energy spectral predictions that can be tested with the new
generation Cherenkov telescope MAGIC.
