Radiative Transfer in Accretion-Disk Winds

IR Web Site 2 Citations 48 References

Search this article

Abstract

type:Article

The radiative transfer equation in an accretion-disk wind is examined both analytically and numerically under a plane-parallel approximation in the subrelativistic regime of .v=c/1, where v is the wind vertical velocity. The emergent intensity is analytically obtained for the case of a large optical depth, where the flow speed and the source function are almost constant. The usual limb-darkening effect, which depends on the direction cosine at the zero-optical depth surface, does not appear, since the source function is constant. Because of the vertical motion of winds, however, the emergent intensity exhibits a velocity-dependent limb-darkening effect, which comes from Doppler and aberration effects. Radiative moments and emergent intensity were also numerically obtained. When the flow speed is small (v 0:1c), the radiative structure resembles that of a static atmosphere, where the source function is proportional to the optical depth, and the usual limb-darkening effect exists. When the flow speed becomes large, on the other hand, the flow speed attains the constant terminal one, and the velocity-dependent limb-darkening effect appears. We thus carefully treat and estimate the wind luminosity and limb-darkening effect, when we observe an accretion-disk wind.

Journal

Citations (2)*help

See more

References(48)*help

See more

Keywords

Details 詳細情報について

Report a problem

Back to top