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

規(guī)章

A Thermo-Radiatively Driven, Analytical 2-D Model for Stellar Outflowssas 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).

SOBER

Numerical Simulations of Dust-Driven AGB Winds: A Two-Fluid Modelm, 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:..

血友病

無目標

The Solar Wind in Three Dimensionsin 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.

雜役

Variable Winds in Yellow Supergiantsates were calculated by assuming the solar abundance for barium. Our mass-loss rates are sensitive to this assumption, because the abundance of s-processed elements like barium can be significantly increased after the third dredge-up phase.

Jacket

Conference proceedings 1998s to present the state of the art in a concise 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.

comely

Using ISO to Probe the Acceleration of Wolf-Rayet Windserved with the ISO SWS for the stars WR 134 (WN6) and WR 136 (WN6). Of these, the 2.83 .m line probes deepest into the wind owing to the dominant free-free opacity. The winds of both WR 134 and WR 136 have attained only 75% of their respective terminal speeds at the radii where the 2.83 .m line is formed.

蘆筍

A Critical Evaluation of Mass-Loss Rates and Wind Properties of Evolved Late-Type Starsf the line profiles to the wind parameters ., .., .., β, and ... We are finding that while accurate and reliable values of . are difficult to obtain, the most reliable values come from the application of two or more independent techniques.

Adenoma

Baffle

Variable Dust Emission Observed in Mirass alternately to evaporate and re-condense in the inner parts of their shells. Hence, emission from the dust will vary during the pulsational cycle. These variations have been observed in the low-resolution spectra (LRS) of Miras obtained by IRAS.