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Binary systems of Population III can evolve to microquasars when one of thestars collapses into a black hole. When the compact object accretes matter at arate greater than the Eddington rate, powerful jets and winds driven by strongradiation pressure should form. We investigate the structure of the jet-windsystem for a model of Population III microquasar on scales beyond the jet-windformation region. Using relativistic hydrodynamic simulations we find that theratio of kinetic power between the jet and the disk wind determines theconfiguration of the system. When the power is dominated by the wind, the jetfills a narrow channel, collimated by the dense outflow. When the jet dominatesthe power of the system, part of its energy is diverted turning the wind into aquasi-equatorial flow, while the jet widens. From the results of oursimulations, we implement semi-analytical calculations of the impact of thequasiequatorial wind on scales of the order of the size of the binary system.Our results indicate that Population III microquasars might inject gamma raysand relativistic particles into the early intergalactic medium, contributing toits reionization at large distances from the binary system.

Equatorial outflows driven by jets in Population III microquasars