Cloudy Accretion Disks

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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 Gamma_eff increases, where Gamma_eff is defined as Gamma_eff =(theta/theta_T)(m_p/m)(L_d/L_E), theta and m being the particle cross-section and mass, respectively, theta_T and m_p the Thomson cross-section and proton mass, respectively, and L_d and L_E the disk and Eddington luminosities, respectively. When Gamma_eff 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 Gamma_eff 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 Gamma_eff, the temperature distribution of the cloud resembles the standard disk. As Gamma_eff 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 Gamma_eff.

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