Equatorial Wind Compression Effects Across the HR-Diagram

Details Equatorial Wind Compression Effects Across the HR-Diagram Equatorial Wind Compression Effects Across the HR-Diagram

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.2114i&link_type=abstract

American Astronomical Society, 186th AAS Meeting, #21.14; Bulletin of the American Astronomical Society, Vol. 27, p.840

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Bjorkman & Cassinelli (1993) developed a kinematical description for the supersonic winds from rotating stars. In their analytical model, material from the polar flow is deflected toward the equator resulting in an equatorial wind compression (the Wind-Compressed Disk model). Using a standard beta -velocity law, we investigate the sensitivity of the wind distortion to the wind acceleration by varying the velocity exponent, beta . As examples, we consider applications of the model to B[e] stars, Asymptotic Giant Branch stars, and novae. Using a shallow wind acceleration with beta =3, equatorial to polar density contrasts of 3 or more (which we call Wind-Compressed Zone models) result in all of these stars for stellar rotations of only 10%-20% critical. Consequently, if the stellar winds are accelerated over radially extended regions, then moderate stellar rotations may be sufficient to explain the aspherical mass-loss observed in some members of these stellar classes.

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