Titlebook: Mass Loss and Evolution of O-Type Stars; P. S. Conti,C. W. H. Loore Book 1979 International Astronomical Union 1979 spectroscopy.star.stel

代替

高度赞扬

H Alpha Variations in Two Mass Losing Starsatory. The observations have been made at the Cassegrain focus of the 1.93 m. The dispersion of the spectrograph was 17 Å.mm. at H. and the slit was 300µ wide. The detector was a cooled SIT TV camera tube commercially available under the name of “Nocticon”.Details on the observing technique have bee

ticlopidine

Short Term Variability of Line Strengths in Some of and WR Starsate to phenomena which are reasonably well understood, as for example the Beta Canis Majoris stars, which are short period pulsators. In other cases, such as the Of and WR stars, the mechanism responsible for the variation is not fully understood. Models proposed to explain this variability include:

火花

epinephrine

不持续就爆

Enervate

男学院

Wolf-Rayet Stars in the Magellanic Clouds for WR stars in the SMC had ever been made, a survey was carried out with the ESO Objective Prism Astrograph which resulted in the identification of 4 new WR stars of the WN type, afterwards confirmed by slit spectroscopy. In the LMC, two fields were also observed and 13 new faint WR stars detected

Accolade

Stellar Outflow: Relative Motions of Nebulae and of Starsly formed hot stars and the surrounding interstellar medium are sufficiently different so that typical H II regions should consist of material which is continually being replaced by the ambient medium and which should therefore possess the velocity of the medium rather than that of the star. Obvious

使成整体

An Ultraviolet View of Stellar Windsrtially evident from earlier ground-based observations. Ultraviolet resonance lines of a variety of ionization stages of several common elements provide a comprehensive probe of the low-density, extended winds. Three general types of information have been derived from ultraviolet spectroscopy of mas