Magnetically driven accretion in the Kerr metric. 3. Unbound outflows
Jul, 2004
33 pages
Published in:
- Astrophys.J. 620 (2005) 878-888
e-Print:
- astro-ph/0407092 [astro-ph]
DOI:
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Abstract: (arXiv)
We have carried out fully relativistic numerical simulations of accretion disks in the Kerr metric. In this paper we focus on the unbound outflows that emerge self-consistently from the accretion flow. These outflows are found in the axial funnel region and consist of two components: a hot, fast, tenuous outflow in the axial funnel proper, and a colder, slower, denser jet along the funnel wall. Although a rotating black hole is not required to produce these unbound outflows, their strength is enhanced by black hole spin. The funnel-wall jet is excluded from the axial funnel due to elevated angular momentum, and is also pressure-confined by a magnetized corona. The tenuous funnel outflow accounts for a significant fraction of the energy transported to large distances in the higher-spin simulations. We compare the outflows observed in our simulations with those seen in other simulations.- accretion, accretion disks
- black hole physics
- ISM: jets and outflows
- MHD
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