Winds from the inner region of accretion disks

Details Winds from the inner region of accretion disks Winds from the inner region of accretion disks

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47..317n&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 47, no. 3, p. 317-321

Astronomy and Astrophysics

Astronomy

6

Accretion Disks, Black Holes (Astronomy), Cylindrical Shells, Mass Flow, Mass Flow Rate, Neutron Stars, Stellar Winds, Angular Momentum, Boundary Conditions, Equations Of Motion, Temperature Distribution, Velocity Distribution

Scientific paper

Steady disk winds, or jets, from inner region of a geometrically thin accretion disk were studied under the assumption that the wind flow is confined within a hollow cylindrical-shell region. By using the cold-wind approximation, in which the variation of the flow properties perpendicular to the streamline is neglected, we integrated the physical quantities over the direction perpendicular to the wind flow. Then, the configuration of streamlines as well as the density and velocity profiles along the streamline were solved simultaneously. We have found that a wind is able to flow vertically. That is, as the cross-sectional area of the wind flow increases along with an increase in the distance from the disk, both the velocity and density decrease, and, accordingly, the Mach number increases with distance. At a sufficiently large height, z much greater than rc0 greater than or = 5 rg, where the wind reaches its terminal speed (0.2-0.5 times the initial velocity, depending on the parameters), the cross-sectional area varies as A proportional to z3/2, the density as rho proportional to z-3/2, the sound velocity as cs proportional to z-0.5, and the Mach number M(= nu/cs) as proportional z0.5. Such a disk wind from the inner accretion disk accounts for the energetic jets from a transient X-ray source and the transient appearance of pair annihilation lines in X-ray Nova Muscae 1991.

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