Titlebook: Radio Recombination Lines; Proceedings of a Wor P. A. Shaver Conference proceedings 1980 D. Reidel Publishing Company, Dordrecht, Holland 1

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書目名稱Radio Recombination Lines影響因子(影響力)




書目名稱Radio Recombination Lines影響因子(影響力)學(xué)科排名




書目名稱Radio Recombination Lines網(wǎng)絡(luò)公開度




書目名稱Radio Recombination Lines網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Radio Recombination Lines被引頻次




書目名稱Radio Recombination Lines被引頻次學(xué)科排名




書目名稱Radio Recombination Lines年度引用




書目名稱Radio Recombination Lines年度引用學(xué)科排名




書目名稱Radio Recombination Lines讀者反饋




書目名稱Radio Recombination Lines讀者反饋學(xué)科排名

大炮

Systematic Variation of the Helium Ionization in Galactic HII Regionse for larger radii. This behavior can be interpreted as reflecting a general decrease of the He abundance with the galactic radius (similar to that also found for planetary nebulae; Torres-Peimbert and Peimbert, 1977) plus a reduction of the ionization in the inner parts of the Galaxy. The crucial aspect is that the observations

辮子帶來幫助

Carbon Radio Recombination Line Emission from Dark Clouds source and as an extended source of far infrared thermal dust emission; the CII region coincides with a localized region of enhanced molecular line emission. We summarize the physical properties (temperature and density) of the CII regions as derived from the recombination line observations and comment on prospects for further research.

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ARC

charisma

Interpretation of HII Region Radio Recombination Linesno need for another review in the traditional sense. There does however seem to be a certain amount of confusion, at least among observers, as to whether or not theory and observations are consistent with one another. One problem is that simple models of the recombination line transfer do not appear

宮殿般

reptile

Radio Recombination Lines from Planetary Nebulaen (Terzian 1973, 1978). Only in recent years it has been possible to detect these lines with adequate signal-to-noise ratios. The largest radio telescopes have been used for such observations with long integration times. Successful results have been obtained for Hnα lines with n ≤ 110, and only uppe

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