Clientele
发表于 2025-3-21 19:24:43
书目名称Mass Loss and Evolution of O-Type Stars影响因子(影响力)<br> http://figure.impactfactor.cn/if/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars影响因子(影响力)学科排名<br> http://figure.impactfactor.cn/ifr/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars网络公开度<br> http://figure.impactfactor.cn/at/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars网络公开度学科排名<br> http://figure.impactfactor.cn/atr/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars被引频次<br> http://figure.impactfactor.cn/tc/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars被引频次学科排名<br> http://figure.impactfactor.cn/tcr/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars年度引用<br> http://figure.impactfactor.cn/ii/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars年度引用学科排名<br> http://figure.impactfactor.cn/iir/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars读者反馈<br> http://figure.impactfactor.cn/5y/?ISSN=BK0625237<br><br> <br><br>书目名称Mass Loss and Evolution of O-Type Stars读者反馈学科排名<br> http://figure.impactfactor.cn/5yr/?ISSN=BK0625237<br><br> <br><br>
resilience
发表于 2025-3-21 20:29:09
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eucalyptus
发表于 2025-3-22 02:23:31
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Connotation
发表于 2025-3-22 06:36:20
Analysis of UV Spectrophotometric Observations for O-type Starsesolution of 35–40 A, depending on the channel, in the wavelength range 1350–2550 A. The Copernicus catalogue gives spectra between 1000 and 1450 A for 17 O-type stars, with low reddening, at 0.2 A resolution.
evince
发表于 2025-3-22 10:32:52
Wolf-Rayet Stars in the Magellanic Clouds4 new WR stars of the WN type, afterwards confirmed by slit spectroscopy. In the LMC, two fields were also observed and 13 new faint WR stars detected. The results presented here mainly concern the SMC WR stars.
landfill
发表于 2025-3-22 13:53:10
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beta-cells
发表于 2025-3-22 18:05:27
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幻影
发表于 2025-3-22 23:57:21
C IV Resonance Line Profiles in O Starsen 3 and 4 Å, as well as thousands of stars at longer wavelengths and correspondingly lower resolution. An atlas of spectra for types O4 to B5 is illustrated in Paper I. That figure shows that the P Cygni profile is a characteristic of all supergiants earlier than B3 and main sequence stars earlier than 08.
种族被根除
发表于 2025-3-23 05:24:44
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共同确定为确
发表于 2025-3-23 07:27:19
The O Stars: Optical Reviewss rates may account for a large fraction of the new matter injected into the interstellar medium, and they probably power some significant fraction of the hard X-ray sources in the galaxy, by virtue of the fact that a companion can become a neutron star a) without disrupting the binary and b) while the companion is still a mass losing O star.