Titlebook: Effects of Mass Loss on Stellar Evolution; IAU Colloquium no. 5 C. Chiosi,R. Stalio Book 1981 D. Reidel Publishing Company, Dordrecht, Holl

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The Velocity Characteristics of WR Stellar Winds transitions of common ions and generally occur in the UV, and typical resonance lines of SiIV, CIV, NV and OVI are well known P-Cygni signatures of stellar winds in luminous OB stars. Analyses of these profiles can lead to important information concerning the velocity, density and temperature struc

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Mass Loss from Central Stars of Planetary Nebulae± 100 km s.. Our preliminary evaluation of the associated mass loss rate gives 10. M. yr.. Other planetary nebulae nuclei are studied with low resolution IUE spectra and indications are found of mass loss rates consistent with the above value.

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Radio Observations and the Mass Flow Rate of α CYG (A2Ia)icted a 10 GHz radio flux of 2.z mJy. On the other hand Praderie et al. (1980) derived a considerable lower mass loss rate of 1.1 10. ≤ . ≤ 7 10. M. yr. from a curve of growth analysis of the envelope ultraviolet Fell-lines of α Cyg. Radio observations are desirable to make a decision about these di

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Observational Evidences of Stellar WindW) and its interaction with the interstellar medium (ISM). Lines arising from excited levels connected radiatively to the ground level tend to be more frequent and/or strong compared to those arising from radiatively forbidden levels of similar excitation as expected from radiatively driven wind. Th

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The Radial Velocity Variations in IC 418spectrograms were taken with the image-tube spectrographs of the 1-m and 4-m telescopes at the Cerro Tololo Inter-American Observatory (CTIO). The emulsion was always IIIa-J baked in “forming gas” (N2+H2). The “blue” spectrograms extend from 3600 to 5000 Å at 45 Å mm.; the “red” ones extend from 500