Cloudy Accretion Disks

Details Cloudy Accretion Disks Cloudy Accretion Disks

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55.1115k&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.6, pp. 1115-1120

Astronomy and Astrophysics

Astronomy

2

Accretion, Accretion Disks, Galaxies: Active, Protoplanetary Disks, X-Rays: Stars

Scientific paper

Gas and dust surrounding an accretion disk suffer from the influence of the strong radiation of the disk, to make cloud layers above and below the disk in some cases. We examined a stable configuration of such cloud layers formed around the standard accretion disk. The cloud configuration is drastically changed as the disk effective luminosity Γeff increases, where Γeff is defined as Γeff = (σ / σT) (mp/m) (Ld / LE), σ and m being the particle cross-section and mass, respectively, σT and mp the Thomson cross-section and proton mass, respectively, and Ld and LE the disk and Eddington luminosities, respectively. When Γeff is smaller than 0.8, the cloud configuration is almost parallel to the disk plane, except for the innermost region, where the configuration is inclined to reach the inner edge of the disk. When Γeff exceeds about 0.8, on the other hand, the cloud layer is split at a middle region, where the stable cloud layer disappears. We also calculated the temperature distribution and continuous spectra of the cloud layer. For small Γeff, the temperature distribution of the cloud resembles the standard disk. As Γeff increases, however, the temperature of the inner cloud decreases and that of the outer cloud somewhat increases, due to the irradiation and shadowing effects. As a result, the continuous spectra become softer with Γeff.

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