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 \Gamma \sim 100 - 1000 .
We showed that radiatively inefficient AGN , such as M87 , are synchrotron-cooling limited to \Gamma \sim 2 - 10 .
Radiatively efficient x-ray binaries , such as GRS1915+105 , are Compton-drag limited to \Gamma \lesssim 2 , but the jet may be destroyed by Compton drag .
However , the Poynting-baryon jet is a collimated outflow with \Gamma \sim 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 \Gamma \sim 100 - 1000 and a Gaussian structure .
Temporal variability of the jet is dominated by toroidal field instabilities for \gtrsim 10 ^ { 2 } gravitational radii .
A broader Poynting-baryon jet with \Gamma \sim 1.5 could contribute to a supernova .