是英寸
发表于 2025-3-21 19:39:25
书目名称Binary and Multiple Stars as Tracers of Stellar Evolution影响因子(影响力)<br> http://impactfactor.cn/if/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution影响因子(影响力)学科排名<br> http://impactfactor.cn/ifr/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution网络公开度<br> http://impactfactor.cn/at/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution网络公开度学科排名<br> http://impactfactor.cn/atr/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution被引频次<br> http://impactfactor.cn/tc/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution被引频次学科排名<br> http://impactfactor.cn/tcr/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution年度引用<br> http://impactfactor.cn/ii/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution年度引用学科排名<br> http://impactfactor.cn/iir/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution读者反馈<br> http://impactfactor.cn/5y/?ISSN=BK0186289<br><br> <br><br>书目名称Binary and Multiple Stars as Tracers of Stellar Evolution读者反馈学科排名<br> http://impactfactor.cn/5yr/?ISSN=BK0186289<br><br> <br><br>
高调
发表于 2025-3-21 23:19:37
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内阁
发表于 2025-3-22 04:19:25
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Torrid
发表于 2025-3-22 05:12:42
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巨头
发表于 2025-3-22 10:53:36
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Licentious
发表于 2025-3-22 13:38:28
Search for Pulsating Stars in Multiple Stellar Systemsy of the turbulent mixing (Vauclair, 1976). A list of possible pulsating companions in visual and spectro-scopic systems with foreseeable period and amplitude is given. Some preliminary results of a spectrophotometric survey begun at the Observatories of Milano — Merate and Bologna — Loiano are also given.
Allergic
发表于 2025-3-22 19:41:58
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COWER
发表于 2025-3-22 22:56:28
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调色板
发表于 2025-3-23 04:06:26
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有毒
发表于 2025-3-23 06:28:31
Rechtsebenen und Regelungsbereiche des IWR,f the cloud are gravitationally unstable, then in the later stage of the evolution only low-mass stars are formed. One can therefore expect that young OB stars are most frequently accompanied by low-mass pre-Main Sequence, stars.