Computer Science
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982iaus...98..453p&link_type=abstract
In: Be stars; Proceedings of the Symposium, Munich, West Germany, April 6-10, 1981. (A83-10301 01-90) Dordrecht, D. Reidel Publi
Computer Science
47
B Stars, Stellar Atmospheres, Stellar Models, Continuous Radiation, Early Stars, Line Spectra, Mass Flow Factors, Polarization (Waves), Radiative Transfer, Spectral Energy Distribution, Stellar Coronas, Stellar Envelopes, Stellar Mass Ejection, Stellar Rotation, Stellar Winds
Scientific paper
A solution to the basic equations governing the structure and dynamics of Be star envelopes is considered as remote now as it was five years ago. In fact, the advent of coronae in stellar wind models has made the entire process even more complex. At present the ad hoc models still furnish the best picture of Be stars. Among the aspects of the Be phenomenon which need clarification are the location of the coronal region and the principles governing V/R variations. With regard to the former, it is noted that at present the limited amount of data indicates no dependence on inclination of the coronal lines. The possibility of having a coronal region at the base of the disk is small since no high outflow velocity is observed in the disk and a high temperature, high density region is ruled out by the polarization observations. With regard to the V/R variation, the elliptic ring model proposed by Huang (1975) has serious difficulty in matching all but the V/R variations. The models of Kriz (1979) are more in accordance with the data but the dynamical arguments in favor of precessing elliptic rings are lost in the case of a disk.
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