lexicographer
发表于 2025-3-21 18:30:28
书目名称Instabilities in Luminous Early Type Stars影响因子(影响力)<br> http://figure.impactfactor.cn/if/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars影响因子(影响力)学科排名<br> http://figure.impactfactor.cn/ifr/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars网络公开度<br> http://figure.impactfactor.cn/at/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars网络公开度学科排名<br> http://figure.impactfactor.cn/atr/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars被引频次<br> http://figure.impactfactor.cn/tc/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars被引频次学科排名<br> http://figure.impactfactor.cn/tcr/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars年度引用<br> http://figure.impactfactor.cn/ii/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars年度引用学科排名<br> http://figure.impactfactor.cn/iir/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars读者反馈<br> http://figure.impactfactor.cn/5y/?ISSN=BK0467906<br><br> <br><br>书目名称Instabilities in Luminous Early Type Stars读者反馈学科排名<br> http://figure.impactfactor.cn/5yr/?ISSN=BK0467906<br><br> <br><br>
供过于求
发表于 2025-3-21 20:29:57
Giant Outbursts of the Eta Carinae - P Cygni TypeDuring such an event, the mass loss rate can be of the order of 0.1 M⨀ yr. for several years. We do not yet understand this phenomenon, partly because most relevant theoretical work has been devoted instead to more familiar, less dramatic stellar winds.
Heterodoxy
发表于 2025-3-22 02:57:03
Radiation Driven Instabilitiescur in the supersonic parts of the winds, where as many as one hundred e-folds of linear growth can occur during a typical outflow time. The nonlinear growth of such instabilities can possibly account for the observed superionization and X-ray emission in these stars. Developments in the linear theory of these instabilities is reviewed.
epinephrine
发表于 2025-3-22 05:57:48
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Arteriography
发表于 2025-3-22 11:37:22
Non Radially Pulsating Wolf-Rayet Stars initial mass 100 M. losing mass through stellar wind. The periods range from half an hour to a feu hours. The duration of this instability phase is rather short, of the order of a feu e-folding times, uhich are of a feu thousand years.
precede
发表于 2025-3-22 14:53:49
https://doi.org/10.1007/978-94-009-3901-1Galaxy; Variation; galaxies; star; stars; stellar; turbulence
Exuberance
发表于 2025-3-22 18:35:12
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小说
发表于 2025-3-23 01:07:23
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饮料
发表于 2025-3-23 03:52:33
Two Comments on the β Cephei Variable 12 LacertaeAccording to a popular notion, the dominant pulsation mode in the g Cephei variables is radial. There is, however, at least one exception to this rule. The exception is 12 Lacertae.
热心助人
发表于 2025-3-23 06:22:57
978-94-010-8232-7D. Reidel Publishing Company, Dordrecht, Holland 1987