Titlebook: Be and Shell Stars; Arne Slettebak (Chairman) Book 1976 Springer Science+Business Media Dordrecht 1976 photometry.spectroscopy.star.stella

septicemia

Prefatory Remarks on Part I: Law and Codeity class III. These stars show similar features in the variation of the intensities, the profiles, and the radial velocities of the shell lines. An attempt has been made to explain the evolution of these unstable features.

MOCK

https://doi.org/10.1007/978-1-4899-0936-7e fait partie de notre programme d’observation qui concerne les étoiles Be de magnitude ≤7 et de déclinaison≥ ?15°. Parmi les étoiles les plus chaudes de ce programme, on peut signaler au moins deux catégories:

枯萎將要

https://doi.org/10.1007/978-1-4613-2823-0ic observations in the 1930’s. The light curve of this star from the end of the 19th century to 1954 was studied by Binnendijk (1949, 1955). Botsula and Sharov (1959) and Sharov (1961) added some old and new observations and continued the light curve up to 1959.

Condense

歡笑

https://doi.org/10.1007/978-94-010-1498-4photometry; spectroscopy; star; stellar

光亮

摘要記錄

Endoscope

Book 1976go, a number of participants expressed the wish to organize a symposium on Be and shell stars. If we wish to identify an official ‘Father of IAU Symposium No. 70‘, it would be Mirek Plavec who, in his capacity as President of IAU Commission 42 (Photometric Double Stars) requested and received the co

貴族

Density

A Study of Be Stars in Clustersf the effect, the extreme Be stars would be excellent probes for studies of spiral structure and would also serve as probes for studies of ages and distances of extragalactic systems..Analysis of the corrected colors of the Be stars in clusters suggests that the Lucy and Solomon (1970) mechanism for