Magnetic flux stabilizing thin accretion disks

Abstract

We calculate the minimal amount of large-scale poloidal magnetic field that has to thread the inner, radiation-over-gas pressure dominated region of a thin disk for its thermal stability. Such a net field amplifies the magnetization of the saturated turbulent state and makes it locally stable. For a $10M_{\odot }$ black hole the minimal magnetic flux is $10^{24}(\dot{M}/{\dot{M}}_{\mathrm{Edd}}{)}^{20/21}\mathrm{G}\cdot \mathrm{c}{\mathrm{m}}^2$. This amount is compared with the amount of uniform magnetic flux that can be provided by the companion star -- estimated to be in the range $10^{22}-10^{24}\mathrm{G}\cdot \mathrm{c}{\mathrm{m}}^2$. If accretion rate is large enough, the companion is not able to provide the required amount and such a system, if still sub-Eddington, must be thermally unstable. The peculiar variability of GRS 1915+105, an X-ray binary with the exceptionally high BH mass and near-Eddington luminosity, may result from the shortage of large scale poloidal field of uniform polarity.

arXiv commentMNRAS Letters, in press

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