A hadronic model for the high-energy gamma-ray emission from the microquasar LS I+61 303

M. ORELLANA; ROMERO, GUSTAVO E; CHRISTIANSEN, H. R.

Congreso; Reunion Anual de la Asociacion Argentina de Astronomia; 2004

Accreting X-ray binary systems that eject collimated relativistic outflows or jets are called microquasars. Recently microquasars had been confirmed to be high energy gamma-ray sources, though the origin of this high energy emission is still debated. 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.