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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 thedense and slow equatorial wind of the Be primary star. We calculate thegamma-ray emission originated in $pp$ interactions between relativistic protonsin the jet and cold protons from the wind. After taking into account opacityeffects on the gamma-rays introduced by the different photons fields, wepresent high-energy spectral predictions that can be tested with the newgeneration Cherenkov telescope MAGIC.Comment: 18 pages,5 figures. Accepted for publication in Astrophysical Journa

Hadronic High‐Energy Gamma‐Ray Emission from the Microquasar LS I +61 303