2000/06/20 by W. Kluźniak, W. Kluzniak, Kluzniak, W. +2 · 2 citations
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #High-pressure geophysics and materials #Phase Equilibria and Thermodynamics #Quantum, superfluid, helium dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0006266
39 pages (incl. fig. captions), 11 figs. (PDF). This is the verbatim text of a ms submitted to the Astrophysical Journal in 1997
arxiv created 2000/06/20 · openalex publication_date 2000/06/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
An analytic solution is presented to the three-dimensional problem of steady axisymmetric fluid flow through an accretion disk. The solution has been obtained through a systematic expansion in the small parameter epsilon =H/R (the ratio of disk thickness to its radial dimension) of the equations of viscous hydrodynamics. The equation of state was assumed to be polytropic. For all values alpha< 0.685 of the viscosity parameter, we find significant backflow in the midplane of the disk occuring at all radii larger than a certain value; however, in the inner regions of the disk the fluid always flows toward the accreting object. The region of backflow is separated from the region of inflow by a surface flaring outwards from a circular locus of stagnation points situated in the midplane of the disk.