General Structure of Steady Accretion Disks with a Magnetic Field

Details General Structure of Steady Accretion Disks with a Magnetic Field General Structure of Steady Accretion Disks with a Magnetic Field

Aug 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979pthph..62..408h&link_type=abstract

Progress of Theoretical Physics, Vol. 62, No. 2, pp. 408-423

Physics

3

Scientific paper

By using the magneto-hydrodynamic equations, we analyze the basic equations describing magnetic accretion disks on the two characteristic surfaces; (a) the Alfvén surface where the accretion velocity is equal to the Alfvén one and (b) the boundary surface where the matter density becomes zero. It is found that the accretion flow always has the super-Alfvénic velocity on the boundary surface, while it can pass from the super-Alfvénic region to the sub-Alfvénic one near the equatorial plane. The transfer of angular momentum by magnetic tension takes place enormously near the Alfvén surface on the boundary, and the Alfvén radius should be much larger than the Keplerian radius in order to obtain stable accretion disks.

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