Disk structure in early-type stellar envelopes

Details Disk structure in early-type stellar envelopes Disk structure in early-type stellar envelopes

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..520h&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 1, 1978, p. 520-526.

Astronomy and Astrophysics

Astronomy

12

Early Stars, Hot Stars, Infrared Astronomy, Stellar Envelopes, Astronomical Models, B Stars, Disks (Shapes), Polarization Characteristics, Stellar Atmospheres, Wolf-Rayet Stars

Scientific paper

It is shown that disk structure can account for some turnovers observed in the infrared excesses of hot stars with extended atmospheres. This theory is applied to the objects most likely to have disks, the Be stars, and explains the correlation of infrared turnovers with large optical polarization. A model for the envelope of the Be star Zeta Tau is developed which accounts for the observed infrared excess and the optical polarization. The envelope has an electron-scattering optical depth of approximately 0.5 to 1.3 and a density gradient r to the -nth power, where n is between 2 and 3. The envelope must be truncated into a disk to produce a polarization from electron scattering, and the optical depth of truncation in the continuum is about 0.1, in good agreement with previous simple models. The large extension of the atmosphere calls into question line-profile analyses using plane-parallel atmospheres and may mean that the true critical rotational velocity is much smaller than assumed. The Be star results suggest that the turnovers observed in Wolf-Rayet spectra are also caused by disk geometry.

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