Relativistic Radiation Hydrodynamical Accretion-Disk Winds

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Abstract

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Accretion-disk winds blowing off perpendicular to a luminous disk are examined within the framework of fully special relativistic radiation hydrodynamics. The wind is assumed to be steady, vertical, and isothermal. Using a velocity-dependent variable Eddington factor, we can solve the rigorous equations of relativistic radiative hydrodynamics, and can obtain radiatively driven winds accelerated up to relativistic speeds. For less-luminous cases, disk winds are transonic types passing through saddle-type critical points, and the final speeds of the winds increase as the disk flux and/or the isothermal sound speed increase. For luminous cases, on the other hand, disk winds are always supersonic, since the critical points disappear due to the characteristic nature of the disk gravitational fields. The boundary between the transonic and supersonic types is located at around FO c 0:1." + p/=. c2/= c, where FO c is the radiative flux at the critical point normalized by the local Eddington luminosity, ." + p/=. c2/ is the enthalpy of the gas divided by the rest-mass energy, and c is the Lorentz factor of the wind velocity at the critical point. In transonic winds, the final speed becomes 0.4–0.8c for typical parameters, while it can reach c in supersonic winds.

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