Astrophysics and Space Science

, Volume 151, Issue 1, pp 81–101 | Cite as

Meridional flow in thick accretion disks

  • Yasushi Kawai


We have studied the effect of the flow in the accretion disk. The specific angular momentum of the disk is assumed to be constant and the polytropic relation is used. We have solved the structure of the disk and the flow patterns of the irrotational perfect fluid.

As far as the obtained results are concerned, the flow does not affect the shape of the configuration in the bulk of the disk, although the flow velocity reaches even a half of the sound velocity at the inner edge of the disk. Therefore, in order to study accretion disk models with the moderate mass accretion rate—i.e.,
$$\dot M \sim 1 \times 10^{ - 4} \left( {\frac{M}{{M_ \odot }}} \right)^2 \left( {\frac{{\rho _{{\text{in}}} }}{{0.1}}} \right)\left( {\frac{{\upsilon _{s,{\text{ in}}} }}{c}} \right)\left( {\frac{{r_{{\text{in}}} }}{{{\text{3}}r_g }}} \right)^2 M_ \odot {\text{yr}}^{ - {\text{1}}} ,$$
it is reasonable to assume that the shape is almost unchanged from that for the disk without flow with small opening angle both at the inner and the outer edge. Here M,M,M, ρin,vs, in, andrin are the mass accretion rate, the mass of the central object, the solar mass, the density on the equatorial plane at the inner boundary, the sound velocity at the inner boundary, and the distance from the central star to the inner boundary of the disk, respectively. However, near the outer edge of the thick disk, the weak density inversion occurs due to the high-flow velocity.


Sound Velocity Equatorial Plane Accretion Disk Outer Edge Open Angle 
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Copyright information

© Kluwer Academic Publishers 1989

Authors and Affiliations

  • Yasushi Kawai
    • 1
  1. 1.Department of Earth Science and Astronomy, College of Arts and SciencesUniversity of TokyoMeguro, TokyoJapan

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