Titlebook: Angular Momentum and Mass Loss for Hot Stars; L. A. Willson,R. Stalio Book 1990 Kluwer Academic Publishers 1990 Population.Variation.astro

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植物学

https://doi.org/10.1007/978-3-030-01542-8 envelope by the stellar disk or depolarization effects due to the finite angular size of the stellar disk. It is assumed that the wind is isothermal and that the electron scattering optical depth is less than unity for all lines of sight. The model is applied to the data for four Be stars which hav

prodrome

The Herbig Ae and Be Stars: Mass and Angular Momentum Losses relatively high mass loss and rotation rates of these stars provide a strong indication that angular momentum loss might play a major role in their evolution, and might even be the source for their paradoxical active phenomena.

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APEX

Intensive Photometric Campaign on Be Stars: Behaviour of Short-Term Periodic Variations and Its Relathis case nearly all the light variation must be due to temperature variations and the model is observationally indistinguishable from the starspot model. We suggest that the localized areas responsible for the light variations are regions of enhanced mass loss.

CROAK

1389-2185 and efficiency of the processes by which angular momentum is redistributed within and lost from stars, and the role that stellar rotation plays in enhancing or driving stellar mass loss. There appears to be a qualitative change in the nature and efficiency of these mechanisms near spectral type FO:

Monolithic

Complement

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Rotation, Pulsation and Atmospheric Phenomena in A—Type Starsulsation, and the possible presence of mass (and angular momentum) loss related to rapid rotation and/or pulsation in these stars. Moreover, some new results derived from the observations of the stars in the far IR are presented.

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