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Jet Formation in Black Hole Accretion Systems II: Numerical Models

Jonathan C. McKinney
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Abstract

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 $Γ\sim 100-1000$. We showed that radiatively inefficient AGN, such as M87, are synchrotron-cooling limited to $Γ\sim 2-10$. Radiatively efficient x-ray binaries, such as GRS1915+105, are Compton-drag limited to $Γ\lesssim 2$, but the jet may be destroyed by Compton drag. However, the Poynting-baryon jet is a collimated outflow with $Γ\sim 1-3$. 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 $Γ\sim 100-1000$ 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 $Γ\sim 1.5$ could contribute to a supernova.

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Jonathan C. McKinney. 2005-06-16. Jet Formation in Black Hole Accretion Systems II: Numerical Models. https://arxiv.org/abs/astro-ph/0506369

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