Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto, 606-8502

The non-LTE state of the hydrogen gas in isothermal transonic decretion disks around a B1V star has been calculated by an iterative method in order to explore the basic physical process in the disk. This dynamical model is characterized by a density law in the equatorial plane of ρ(R) ∝ R^-3.5. The continuous radiation is calculated with the Λ iteration in the integral form, while we adopt a single-flight escape probability for lines. We describe the non-LTE state, the radiation flow and conversion in the disk. We conclude that the stellar Balmer continuum plays a key role in the non-LTE state of the disk. The examination of the local energy gain and loss suggests that the disk temperature has double minima along the equatorial plane in the optically thick case: the intermediate region caused by deficient ultraviolet radiation and the outer Lyman α cooling region. We have also calculated some observable quantities, such as the spectral energy distribution, the UBV colors, the infrared excess and the Balmer line profiles. Our calculations with the mass loss rate less than 10^-10 M yr^-1 reproduce the observed continuum quantities. However, we could not get large Hα emission strength observed in Be stars. We suggest that the density gradient of the Be star disk is slower than that of the isothermal decretion disk.

Accepted by PASJ
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