  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 micron 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, 2.40 +/- 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 +/- 500 K. Least-squares comparisons of synthetic spectral
energy distributions from 1220 A to 3.6 cm with the observations provide
estimates for the effective temperature and the mass-loss rate of 8400 +/- 100
K and 8 +/- 3 E-7 M_sun/yr, 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 Halpha P-Cygni profile with any model parameters over a reasonable
range. This is troubling because the \ha profile is the observational basis for
Wind Momentum-Luminosity Relationship.
