Jet Formation in Black Hole Accretion Systems Ii: Numerical Models

In a companion theory paper, we presented a unified model of jet formation. We suggested that primarily two types of relativistic jets form near accreting black holes: a potentially ultrarelativistic Poynting-dominated jet and a Poynting-baryon jet. We showed that, for the collapsar model, the neutrino-driven enthalpy flux (classic fireball model) is probably dominated by the Blandford-Znajek energy flux, which predicts a jet Lorentz factor of Γ ∼ 100 − 1000. We showed that radiatively inefficient AGN, such as M87, are synchrotron-cooling limited to Γ ∼ 2 − 10. Radiatively efficient x-ray binaries, such as GRS1915+105, are Compton-drag limited to Γ . 2, but the jet may be destroyed by Compton drag. However, the Poynting-baryon jet is a collimated outflow with Γ ∼ 1 − 3. Here we present general relativistic hydromagnetic simulations of black hole accretion with pair creation used to simulate jet formation in GRBs, AGN, and x-ray binaries. Our collapsar model shows the development of a patchy “magnetic fireball” with typically Γ∼ 100 − 1000 and a Gaussian structure. Temporal variability of the jet is dominated by toroidal field instabilities for & 102 gravitational radii. A broader Poyntingbaryon jet with Γ ∼ 1.5 could contribute to a supernova. Subject headings: accretion disks, black hole physics, galaxies: jets, gamma rays: bursts, X-rays : bursts, supernovae: general, neutrinos