Titlebook: Upper Main Sequence Stars with Anomalous Abundances; Proceedings of the 9 C. R. Cowley,M. M. Dworetsky,C. Mégessier Conference proceedings

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書目名稱Upper Main Sequence Stars with Anomalous Abundances影響因子(影響力)




書目名稱Upper Main Sequence Stars with Anomalous Abundances影響因子(影響力)學科排名




書目名稱Upper Main Sequence Stars with Anomalous Abundances網絡公開度




書目名稱Upper Main Sequence Stars with Anomalous Abundances網絡公開度學科排名




書目名稱Upper Main Sequence Stars with Anomalous Abundances被引頻次




書目名稱Upper Main Sequence Stars with Anomalous Abundances被引頻次學科排名




書目名稱Upper Main Sequence Stars with Anomalous Abundances年度引用




書目名稱Upper Main Sequence Stars with Anomalous Abundances年度引用學科排名




書目名稱Upper Main Sequence Stars with Anomalous Abundances讀者反饋




書目名稱Upper Main Sequence Stars with Anomalous Abundances讀者反饋學科排名

CAJ

輕浮女

RENIN

The Magnetic Field and other Parameters of the Chemically Peculiar Starsson it is natural that different investigators are interested in working out and improving methods of determination of B.. Especially great attention attracts the method based on using the multicolor Geneva photometry [1]. Cramer and Maeder have found a dependence between B. and parameter Z of multi

LAST

Does ν Cep Indicate a Non-axisymmetric Dynamo?ws a period of about 5 years. It is unplausible that this magnetic field is a relic since νCep was formed by expansion of a B-star. We claim here that νCep represents a dynamo exciting a magnetic field which in the average strongly deviates from symmetry about the rotation axis.

經典

tympanometry

Ptsd429

Missing Levels and Lines of Astrophysical Importance and singly ionized atoms and t o gi ve rough predictions of missing levels and lines. The amount of data that have been published for these elements after the edition of the Multiple Tables are considerable. For detailed information about sources of new data and compilations the reader is referred

癡呆

Characteristic Absorption Features in the Spectra of Ap-Si Stars Between 1250 and 1850 ?ssible. The contribution of the Si II multiplets is calculated in LTE for a typical overabundance x 10. of silicon. It accounts for only a small part of the observed absorption. Common unidentified structures, smaller than the 1400 ? depression are pointed out.

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