A stellar wind module has been developed for the PHOENIX stellar atmosphere code for the purpose of computing non-LTE , line-blanketed , expanding atmospheric structures and detailed synthetic spectra of hot luminous stars with winds .
We apply the code to observations of Deneb , for which we report the first positive detections of mm and cm emission ( obtained using the SCUBA and the VLA ) , as well a strong upper limit on the 850 \mu m flux ( using the HHT ) .
The slope of the radio spectrum shows that the stellar wind is partially ionized .
We report a uniform-disk angular diameter measurement , \overline { \theta _ { UD } } = 2.40 \pm 0.06 { mas } , from the Navy Prototype Optical Interferometer ( NPOI ) .
The measured bolometric flux and corrected NPOI angular diameter yield an effective temperature of 8600 \pm 500 { K } .
Least-squares comparisons of synthetic spectral energy distributions from 1220 Å to 3.6 cm with the observations provide estimates for the effective temperature and the mass-loss rate of \simeq 8400 \pm 100 K and 8 \pm 3 \times 10 ^ { -7 } M _ { \odot } { yr } ^ { -1 } , respectively .
This range of mass-loss rates is consistent with that derived from high dispersion UV spectra when non-LTE metal-line blanketing is considered .
We are unable achieve a reasonable fit to a typical H \alpha P-Cygni profile with any model parameters over a reasonable range .
This is troubling because the H \alpha profile is the observational basis for Wind Momentum-Luminosity Relationship .