Titlebook: Cyclical Variability in Stellar Winds; Proceedings of the E Lex Kaper,Alexander W. Fullerton Conference proceedings 1998 Springer-Verlag Be

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ESO Astrophysics Symposiahttp://image.papertrans.cn/d/image/241996.jpg

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Wind Variability in the Hypergiant HR 8752 instability region (Nieuwenhuijzen & de Jager 1995). One of the direct consequences of this instability seems to be brief periods of enhanced mass loss that occur when the star comes close to the edge of the instability region during its blueward evolution.

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1431-2433 se form. The proceedings will provide a useful, up-to-date overview of the observations, interpretation, and modelling of the time-dependent mass outflows from all sorts of stars.978-3-662-11392-9978-3-540-68597-5Series ISSN 1431-2433 Series E-ISSN 1611-6143

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Jaydip Singh,Srishti Nagu,Jyotsna Singhsas 1998). Fig. 1 illustrates the logarithmic density contours for our model of the wind of the hypergiant P Cygni, which was computed by using the optically thin radiative force given by Chen & Marlborough (1994) and the acceleration in the envelope determined by Lamers (1986). The results resemble the three-zone envelope of Nugis et al. (1979).

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Chapter 8: Introduction to Verificationm, and energy for an (ideal) gas and a single dust component. Both sets of equations are coupled by the condensation of gas onto dust grains and the transfer of momentum between dust and gas. Condensation is described by the source term in the continuity equations, .., in which .. is the condensation rate and .. > 0:..

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Chapter 8: Introduction to Verification magnetic field geometries are controversial. The time-variability of the outflows is poorly understood; observations of the interactions of jets with the circumstellar medium suggest that the outflows are variable on almost all time scales, but are punctuated by substantial bursts which may be related to FU Ori-like events of high disk accretion.

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Preliminary Test and Stein-Rule Estimatorsin the high-speed wind, the plasma beta there typically being ~3.0. 5. Corotating interaction regions have opposed north-south tilts in the northern and southern hemispheres. 6. A new class of forward-reverse shock pairs associated with over-expanding coronal mass ejections has been identified at high heliographic latitudes.