Titlebook: Structure and Evolution of the Galaxy; Proceedings of the N L. N. Mavridis Conference proceedings 1971 D. Reidel Publishing Company, Dordre

本能

Photometry and Photometric Systems,1963) in which he presented the principal methods of spectral classification based on photometric systems. Finally, the same author has discussed, in another article (1966), the case of narrow-and intermediate-band photometries with special attention to the ., ., ., ., β system. We propose to presen

宴會

Space Distribution and State of Motion of the Early-Type Stars, Open Clusters, Associations and Steed to the theoretical parameters mass, age, chemical composition, rotation… From these relationships we should be able to reach conclusions as to how mass, luminosity, and chemical composition vary with stellar age for different sub-groups of stars, that is, conclusions concerning galactic evolution

Asperity

Conference proceedings 1971tudents a general outline of the field. In addition to the lectures ample time was spent in discussions and personal contacts. In order to simplify the publica- tion it was felt reasonable, however, not to include the discussions in the present volume.

憤慨點吧

浮雕

Interstellar Dust,Interstellar matter is an important component of our Galaxy although its mass may be less than 10% of the whole system. The structure of the Galaxy is strongly affected by the distribution of interstellar matter and its evolution is mainly determined by the amount of interstellar gas and dust which is available for star formation.

追蹤

廢墟

正論

Prestellar Evolution,A symposium on a very similar subject was held in Liège at the beginning of July 1969 and although, for reasons of time and competence, it is quite out of the question for me to try to summarize its proceedings here systematically, I shall certainly refer often to results presented there.

myopia

Evolution of Stellar Clusters and Associations,Star clusters are usually defined as agglomerations of stars in space, whose average projected densities appear to exceed the density of background stars. Cluster members are identified either by parallax measurements or by common motion or also with the help of the color-luminosity diagram established from known members.

FLAG

978-94-010-3077-9D. Reidel Publishing Company, Dordrecht, Holland 1971