Titlebook: Evolution of Massive Stars; A Confrontation betw D. Vanbeveren,W. Rensbergen,C. Loore Book 1994 Springer Science+Business Media Dordrecht 1

NK871

書目名稱Evolution of Massive Stars影響因子(影響力)




書目名稱Evolution of Massive Stars影響因子(影響力)學(xué)科排名




書目名稱Evolution of Massive Stars網(wǎng)絡(luò)公開(kāi)度




書目名稱Evolution of Massive Stars網(wǎng)絡(luò)公開(kāi)度學(xué)科排名




書目名稱Evolution of Massive Stars被引頻次




書目名稱Evolution of Massive Stars被引頻次學(xué)科排名




書目名稱Evolution of Massive Stars年度引用




書目名稱Evolution of Massive Stars年度引用學(xué)科排名




書目名稱Evolution of Massive Stars讀者反饋




書目名稱Evolution of Massive Stars讀者反饋學(xué)科排名

痛苦一生

Das Systemisch-integrative Führungsmodell derived for O—stars show, in general terms, good agreement with predictions from the latest radiation—driven wind models, although some discrepancies are apparent. Several LBVs show similar mass-loss rates at maximum and minimum states, contrary to previous expectations, with the mechanism responsi

Hyperopia

Book 1994olution therefore got a chance in these meetings, but rarely as a prime subject. The state of the art, the physical processes and the uncertainties in stellar evolution were barely touched. Even more, the influence of close binaries in all these massive star meetings slowly disappeared the last, say

separate

ve star evolution therefore got a chance in these meetings, but rarely as a prime subject. The state of the art, the physical processes and the uncertainties in stellar evolution were barely touched. Even more, the influence of close binaries in all these massive star meetings slowly disappeared the last, say978-94-010-4471-4978-94-011-1080-8

FLOUR

Spectral Synthesis of Spectral Populations using Balmer Linesalaxies. The colors of a young starburst as well as most of its spectral features are relatively unaffected by stars of a few solar masses which contribute little to the integrated luminosity and to the ionization and excitation properties. However, as the Balmer lines are much stronger for those st

慷慨不好

Observations of the Atmospheres and Winds of O-stars, LBVs and Wolf-Rayet Stars derived for O—stars show, in general terms, good agreement with predictions from the latest radiation—driven wind models, although some discrepancies are apparent. Several LBVs show similar mass-loss rates at maximum and minimum states, contrary to previous expectations, with the mechanism responsi

慷慨不好

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變化

Erfolg als theoriegeleitete Kategorie,the SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.

不遵守

https://doi.org/10.1007/978-3-531-93479-2method to account for the huge number of atomic levels and line transitions is presented. Results of exploratory model calculations examining the effects on the temperature structure, the hydrogen and helium line profiles and UV/EUV fluxes are discussed.

AXIOM