Titlebook: Variable and Non-spherical Stellar Winds in Luminous Hot Stars; Proceedings of the I Bernhard Wolf,Otmar Stahl,Alex W. Fullerton Conference

厭煩

Observing hot stars in all four stokes parameters,aneous manner. We briefly outline the technical design of the polarimeter unit and the linear algebraic Mueller calculus for obtaining polarization parameters of any point source. In addition, practical limitations of the optical elements are discussed. We present first results obtained with our spectropolarimeter for three prototype hot-star.

Project

Throttle

Exonerate

Rotationally modulated winds of O stars,of the underlying star. This rotational modulation is usually attributed to large scale, persistent structures in the wind, which are thought to be generated and maintained by photospheric processes that alter the emergence of the wind from different regions of the stellar surface. In this review, t

Accede

簡略

Disks of classical be stars,of line profiles in the optical and near-IR region were used in the 70th and 80th, the present progress is done also thanks to interferometric and polarimetric observations. These techniques enable to determine the geometrical parameters of the circumstellar disks directly for the first time. They a

修正案

Short and medium term variability of emission lines in selected southern Be stars, stars, . Cen, was found to be in the process of continued gradual recovery of the Hydrogen emitting disk which had been lost from 1977–1989. During the monitoring period numerous line emission outbursts were observed. A generalized pattern of an outburst cycle is derived from observations of differ

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faculty

Polarimetric evidence of non-spherical winds,vidences for non-spherically symmetric structures around Luminous Hot Stars from polarimetry and what we can learn with this technique. Polarimetry has added a new dimension to the study of the envelopes of Luminous Blue Variables, Wolf-Rayet stars and B[e] stars, all of which are discussed in some

軍械庫

Wolf-rayet wind models: Photometric and polarimetric variability,ve localized, enhanced density regions (blobs). Our model is based on a Monte Carlo code that treats all Stokes parameters of the radiation bundle. This study indicates that the blobs must have sizes comparable to the stellar dimension and be near the base of the envelope. These blobs can be interpr