Magnetically Advected Winds
arXiv:1705.11026 · doi:10.1093/mnrasl/slx123
Abstract
Observations of X-ray absorption lines in magnetically driven disk winds around black hole binaries and active galactic nuclei yield a universal radial density profile rho proportional to r^{-1.2} in the wind. This is in disagreement with the standard Blandford & Payne profile rho_BP proportional to r^{-1.5} expected when the magnetic field is neither advected nor diffusing through the accretion disk. In order to account for this discrepancy, we establish a new paradigm for magnetically driven astrophysical winds according to which the large scale ordered magnetic field that threads the disk is continuously generated by the Cosmic Battery around the inner edge of the disk and continuously diffuses outward. We obtain self-similar solutions of such magnetically advected winds (MAW) and discuss their observational ramifications.
5 pages, 1 figures, accepted for publication in Monthly Notices Letters
References in corpus (7)
- On the Magnetic Prandtl Number Behavior of Accretion Disks
- Magnetically-Driven Accretion-Disk Winds and Ultra-Fast Outflows in PG1211+143
- Advection/Diffusion of Large-Scale B-Field in Accretion Disks
- Detection of high velocity outflows in Seyfert 1 galaxy Mrk 590
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- Accretion disk radiation dynamics and the cosmic battery
- Magnetically Advected Winds
Cited by in corpus (6)
- Magnetically-driven jets and winds from weakly magnetized accretion disks
- Magnetized Disk-Winds in NGC 3783
- Magnetohydrodynamic Winds Driven by the Line Force from the Standard Thin Disk around Supermassive Black Holes. I. The Case of Weak Magnetic Field
- Magnetically Advected Winds
- BALQSO Spectra Explained by Shock Disruption of Galactic Clouds
- The immediate environment of an astrophysical black hole