Titlebook: Astrophysical and Laboratory Plasmas; A Festschrift for Pr A. J. Willis,T. W. Hartquist Book 1996 Springer Science+Business Media Dordrecht

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書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas影響因子(影響力)




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas影響因子(影響力)學(xué)科排名




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas網(wǎng)絡(luò)公開(kāi)度




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas網(wǎng)絡(luò)公開(kāi)度學(xué)科排名




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas被引頻次




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas被引頻次學(xué)科排名




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas年度引用




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas年度引用學(xué)科排名




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas讀者反饋




書(shū)目名稱(chēng)Astrophysical and Laboratory Plasmas讀者反饋學(xué)科排名

regale

Blanch

adhesive

MIR

Chemically Peculiar Hot Stars in chemically peculiar stars, with an emphasis on insights provided by a generation of ultraviolet observations obtained with the . satellite. The paper concludes with an overview of the radiative diffusion mechanism which has been proposed as an explanation of the chemically peculiar phenomenon.

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榮幸

Particle Attraction and Gravity the highest levels of mass loss amongst early-type stars: mass loss rates, typically, lie in the range [1–10] × 10...yr.. Radiation pressure—driven winds incorporating multi-scattering in high ionisation—stratified winds may cause these levels, but additional mechanisms may also be needed.

Infant

Wolf—Rayet Stars the highest levels of mass loss amongst early-type stars: mass loss rates, typically, lie in the range [1–10] × 10...yr.. Radiation pressure—driven winds incorporating multi-scattering in high ionisation—stratified winds may cause these levels, but additional mechanisms may also be needed.

體貼

Foundation Actionscript 3.0 Animationcorona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales — at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle.

Congestion

Foundation Actionscript 3.0 Animationpower them, and the accretion processes which convert this into electromagnetic radiation. Particular attention is paid to the topics of mass transfer fluctuations and of the accretion by magnetic compact stars.