Luminous hot accretion disks

Feng Yuan

doi:10.1046/j.1365-8711.2001.04258.x

paper

Luminous hot accretion disks

arXiv:astro-ph/0009207 · doi:10.1046/j.1365-8711.2001.04258.x

Abstract

We find a new two-temperature hot branch of equilibrium solutions for stationary accretion disks around black holes. In units of Eddington accretion rate defined as $10 L_{Edd} / c^{2}$ , the accretion rates to which these solutions correspond are within the range $\dot{m}_1 \la \dot{m} \la 1$, here $m ˙_{1}$ is the critical rate of advecti $. I n t h eseso l u t i o n s, t h ee n er g y l ossr a t eo f t h e i o n s b y C o u l o mb e n er g y t r an s f er b e tw ee n t h e i o n s an d e l ec t r o n s i s l a r g er t han t h e v i sco u s l y h e a t in g r a t e an d i t i s t h e a d v ec t i v e h e a t in g t o g e t h er w i t h t h e v i sco u s d i ss i p a t i o n t ha t ba l an ces t h e C o u l o mb coo l in g o f i o n s . W h e n$ \dot{m}_1 \la \dot{m} \la \dot{m}_2 $, w h er e$ \dot{m}_2 \sim 5 \dot{m}_1 < 1 $, t h e a ccr e t i o n f l o w r e main s h o tt h r o ug h o u tt h e d i s k . W h e n$ \dot{m}_2 \la \dot{m}\la 1 $, C o u l o mbin t er a c t i o n w i l l coo l t h e inn er r e g i o n o f t h e d i s k w i t hina cer t ain r a d i u s ($ r_{\rm tr} \sim$ several -- tens of Schwarzschild radii or larger depending on the accretion rate and the outer boundary condition) and the disk will collapse onto the equatorial plane and form an optically thick cold annulus. Compared to ADAF, these hot solutions are much more luminous because of the high accretion rate and efficiency, therefore, we name them luminous hot accretion disks.

12 pages, 6 figures, uses mn.sty, the final version accepted by MNRAS, discussion extended to emphasize the difference between ADAF and my model

Luminous hot accretion disks

Abstract

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