Herbaceous
发表于 2025-3-21 19:32:46
书目名称Mass Loss from Stars影响因子(影响力)<br> http://figure.impactfactor.cn/if/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars影响因子(影响力)学科排名<br> http://figure.impactfactor.cn/ifr/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars网络公开度<br> http://figure.impactfactor.cn/at/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars网络公开度学科排名<br> http://figure.impactfactor.cn/atr/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars被引频次<br> http://figure.impactfactor.cn/tc/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars被引频次学科排名<br> http://figure.impactfactor.cn/tcr/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars年度引用<br> http://figure.impactfactor.cn/ii/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars年度引用学科排名<br> http://figure.impactfactor.cn/iir/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars读者反馈<br> http://figure.impactfactor.cn/5y/?ISSN=BK0625239<br><br> <br><br>书目名称Mass Loss from Stars读者反馈学科排名<br> http://figure.impactfactor.cn/5yr/?ISSN=BK0625239<br><br> <br><br>
Arthritis
发表于 2025-3-21 23:39:33
The Wolf-Rayet Stars and Mass Losss incontrovertible that Wolf-Rayet stars are losing mass, a typical rate of mass loss being near 10... per year. The outward directed velocity of the expanding shell has been estimated for 10 stars. The largest value found is 2500 km/sec; most values lie between 1000 and 1500 km/sec. Two outstanding
可卡
发表于 2025-3-22 02:02:18
Mass Loss from P Cygnishvili and Kharadze that P Cygni is a WUMa type system. It is found that many of the absorption lines are double, the hydrogen absorption lines even triple. This is attributed to line formation in different shells. In the outer shell variations with a period of 114 days lead to observed radial-veloc
起皱纹
发表于 2025-3-22 05:25:19
Rocket Observations of Mass Loss from Hot StarsRayet stars and OB supergiants. Velocity shifts as high as —3000 km sec. have been measured for the short-wavelength edges of some of the lines. Estimates of the rates of mass loss range from 10. to 10... year..
Myosin
发表于 2025-3-22 10:16:21
Intrinsic Polarization for Objects with Extended Atmospheres particularly the decrease in polarization in the ultraviolet, is explained by scattering from electrons in an asymmetrical envelope together with self-absorption in a hydrogen plasma..Red variable stars show large polarizations in the ultraviolet. Unlikely configurations of the scattering envelope,
赤字
发表于 2025-3-22 15:04:01
Mass Loss from OB Supergiantselopes of the stars. Illustrations are given from two southern stars. A method of computing strong line profiles in extended moving atmospheres is outlined, and it is shown how these profiles support the proposed atmospheric structure of the stars. Preliminary general conclusions are drawn on the ph
NEG
发表于 2025-3-22 17:32:00
Evidence for Mass Loss from the F-Type Supergiant, 89 Herculisstar is remarkable in that some of the blue-displaced circumstellar absorption features have velocities of 150 km/sec. This is very close to the estimated escape velocity at the stellar surface of 200 km/sec. It is probable that the rate of mass loss is too small to affect the subsequent evolution o
不要严酷
发表于 2025-3-23 00:02:33
A New Outburst of the Shell Star 48 Librae of the Balmer lines are sharp on the longward side but winged shortward and emission is visible for the first few series members. The Feii lines show similar asymmetry and the strongest lines are accompanied by emission. The radial velocity shown by different lines varies from about — 130 km/sec to
粗鲁性质
发表于 2025-3-23 01:47:48
Microturbulence in Stellar Atmospheres Methodic Remark Obviously, this action must be clarified, before the influence of large-scale turbulence or streams on profiles can be treated. Moreover, we will see that a generalization will allow us to account for emission features, whether they originate from a shell or a circumstellar medium.
变量
发表于 2025-3-23 08:52:58
Recent Studies of Models for Unstable Starslations of stellar models that include these unstable stages and discusses some of their possible consequences..The influence of neutrino emission becomes very important during the helium shell-burning stage for stars more massive than 1... Calculations are described that illustrate the influence of