Squeezing of toroidal accretion disks
arXiv:1301.1557 · doi:10.1209/0295-5075/101/19001
Abstract
Accretion disks around very compact objects such as very massive Black hole can grow according to thick toroidal models. We face the problem of defining how does change the thickness of a toroidal accretion disk spinning around a Schwarzschild Black hole under the influence of a toroidal magnetic field and by varying the fluid angular momentum. We consider both an hydrodynamic and a magnetohydrodynamic disk based on the Polish doughnut thick model. We show that the torus thickness remains basically unaffected but tends to increase or decrease slightly depending on the balance of the magnetic, gravitational and centrifugal effects which the disk is subjected to.
6 pages, 17 figures, to appear in EPL
References in corpus (4)
- Magnetized Tori around Kerr Black Holes: Analytic Solutions with a Toroidal Magnetic Field
- Dynamics of magnetized relativistic tori oscillating around black holes
- Bridging the gap between stellar-mass black holes and ultraluminous X-ray sources
- On the Polish doughnut accretion disk via the effective potential approach
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- Effect of the toroidal magnetic field on the runaway instability of relativistic tori
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- Dragged surfaces. On the accretion tori in the ergoregion
- Jet collision with accreting tori around SMBHs. GRHD and light surfaces constraints in aggregates of misaligned tori
- Embedded BHs and multipole globules: Clustered misaligned thick accretion disks around static SMBHs
- General features of the linear crystalline morphology of accretion disks