標題: Titlebook: Astrophysical and Laboratory Plasmas; A Festschrift for Pr A. J. Willis,T. W. Hartquist Book 1996 Springer Science+Business Media Dordrecht [打印本頁] 作者: 請回避 時間: 2025-3-21 16:53
書目名稱Astrophysical and Laboratory Plasmas影響因子(影響力)
書目名稱Astrophysical and Laboratory Plasmas影響因子(影響力)學(xué)科排名
書目名稱Astrophysical and Laboratory Plasmas網(wǎng)絡(luò)公開度
書目名稱Astrophysical and Laboratory Plasmas網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Astrophysical and Laboratory Plasmas被引頻次
書目名稱Astrophysical and Laboratory Plasmas被引頻次學(xué)科排名
書目名稱Astrophysical and Laboratory Plasmas年度引用
書目名稱Astrophysical and Laboratory Plasmas年度引用學(xué)科排名
書目名稱Astrophysical and Laboratory Plasmas讀者反饋
書目名稱Astrophysical and Laboratory Plasmas讀者反饋學(xué)科排名
作者: regale 時間: 2025-3-21 22:47 作者: Blanch 時間: 2025-3-22 02:25 作者: adhesive 時間: 2025-3-22 07:10 作者: MIR 時間: 2025-3-22 12:10
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.作者: 音樂會 時間: 2025-3-22 14:28 作者: 榮幸 時間: 2025-3-22 17:05
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.作者: Infant 時間: 2025-3-23 00:55
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.作者: 體貼 時間: 2025-3-23 05:08
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.作者: Congestion 時間: 2025-3-23 07:28
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.作者: Accolade 時間: 2025-3-23 09:58 作者: 發(fā)出眩目光芒 時間: 2025-3-23 14:53 作者: decipher 時間: 2025-3-23 19:37 作者: Graduated 時間: 2025-3-24 02:03
Using an Animation and Effects Library,ing of material between different nuclear burning zones in evolved stars and turbulent boundary layers (which are present in and influence the structures and evolution of all diffuse astrophysical sources) are treated.作者: 幼稚 時間: 2025-3-24 06:10
Foundation ActionScript 3.0 Image Effectshat self-consistent models of the dynamical and chemical evolution of collapsing cores, coupled to multiple high resolution line observations, will provide definitive evidence for the presence of infall in these objects.作者: Synapse 時間: 2025-3-24 06:33 作者: nocturia 時間: 2025-3-24 13:29 作者: 疲勞 時間: 2025-3-24 18:48 作者: Picks-Disease 時間: 2025-3-24 21:01
The Chromosphere-Corona Transition Region in Late-Type Starsof stellar transition regions show common behaviour as well as systematic trends. The basic methods used in making models of the transition region are set out. Observations relating to inhomogeneities in the solar transition region are summarized. The structure and energy balance of stellar transition regions and the trends emerging are discussed.作者: 諂媚于性 時間: 2025-3-25 01:18 作者: EWE 時間: 2025-3-25 06:51 作者: ectropion 時間: 2025-3-25 09:51 作者: KEGEL 時間: 2025-3-25 11:41 作者: AIL 時間: 2025-3-25 16:27 作者: Insufficient 時間: 2025-3-25 20:27
Overview: 978-90-481-4729-8978-94-017-0803-6作者: 行為 時間: 2025-3-26 01:17
Foundation Actionscript 3.0 Animationof stellar transition regions show common behaviour as well as systematic trends. The basic methods used in making models of the transition region are set out. Observations relating to inhomogeneities in the solar transition region are summarized. The structure and energy balance of stellar transition regions and the trends emerging are discussed.作者: olfction 時間: 2025-3-26 04:56
Inverse Kinematics: Dragging and Reachingf radiativelydriven stellar winds. The theory makes predictions which are shown to be in general accord with the data. We summarize recent results, primarily from the IUE satellite, which demonstrate the importance of time-dependent phenomena in hot-star outflows, and which, in particular, point to effects related to rotational modulation.作者: Favorable 時間: 2025-3-26 12:00
Particle Attraction and Gravityof self-consistent hydrodynamic models for the production of the line-forming regions. We here review such modelling and stress the central role played by shock phenomena induced by winds and explosions on scales ranging from the circumstellar to the intergalactic.作者: Synovial-Fluid 時間: 2025-3-26 13:06
https://doi.org/10.1007/978-94-017-0803-6Accretion; Chromosphere; Corona; Solar; Sun; astronomy; astrophysics作者: aneurysm 時間: 2025-3-26 18:39
978-90-481-4729-8Springer Science+Business Media Dordrecht 1996作者: 眼界 時間: 2025-3-26 22:17 作者: 集中營 時間: 2025-3-27 03:15
Foundation Actionscript 3.0 Animation emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spa作者: exacerbate 時間: 2025-3-27 07:31 作者: arcane 時間: 2025-3-27 11:25
Coordinate Rotation and Bouncing Off Angles This paper presents an informal review of the physical properties of these objects, including their location in the H-R diagram, frequency of incidence, rotation, binarity, magnetic fields, and variability. Part of the discussion is devoted to describing the bizarre surface compositions encountered作者: Instrumental 時間: 2025-3-27 14:25 作者: Femish 時間: 2025-3-27 19:19 作者: GIST 時間: 2025-3-27 22:21
Particle Attraction and Gravitynd stellar wind characteristics and current ideas about their evolutionary status. WR stars are believed to be the evolved descendents of massive O—type stars, in which extensive mass loss reveals successive stages of nuclear processed material: WN stars the products of interior CNO-cycle hydrogen b作者: FID 時間: 2025-3-28 02:07
Foundation Actionscript 3.0 Animations review summarises recent progress in studies of stellar-evolutionary processes that lead to X-ray binaries themselves, the mass transfer rates that power them, and the accretion processes which convert this into electromagnetic radiation. Particular attention is paid to the topics of mass transfer作者: Gum-Disease 時間: 2025-3-28 07:39 作者: Emg827 時間: 2025-3-28 11:59
Foundation ActionScript 3.0 Image Effectsally altered our understanding of the broad-line regions in active galaxies. The constraints these observations impose on the models of the BLRs have been demonstrated here by an attempt to model the BLR of NCC5548, the most intensively monitored AGN. Two models of a BLR, with one having a power law作者: 愚笨 時間: 2025-3-28 15:35 作者: LVAD360 時間: 2025-3-28 19:11 作者: EXULT 時間: 2025-3-28 23:58 作者: 無可爭辯 時間: 2025-3-29 03:59 作者: majestic 時間: 2025-3-29 08:04
Foundation ActionScript 3.0 Image Effectsminosity of the ionizing continuum. The observed centroid or the lag of a line, can be a function of the continuum luminosity..The variability of the profile of the . line in the spectrum of NCC5548 is investigated. This profile is extremely robust and is not significantly affected by changes in the作者: 斑駁 時間: 2025-3-29 13:50 作者: podiatrist 時間: 2025-3-29 15:34 作者: 裙帶關(guān)系 時間: 2025-3-29 22:40
Coronal Heating by Magnetic Reconnectionls known as almost-uniform reconnection and nonuniform reconnection, depending on the boundary conditions. Also, we are beginning to explore the uncharted region of three-dimensional reconnection, where regimes of “spine reconnection” and “fan reconnection” have been discovered. Furthermore, part of作者: conscribe 時間: 2025-3-30 01:01 作者: maladorit 時間: 2025-3-30 05:41
Levitationevitation occurs when the forces due to radiation pressure are larger than those due to gravitation..The paper describes some recent work on the calculation of the radiative forces using atomic data obtained in the course of the work of the Opacity Project..Large abundance anomalies are observed for作者: Minikin 時間: 2025-3-30 09:30
Winds of Luminous OB Starsf radiativelydriven stellar winds. The theory makes predictions which are shown to be in general accord with the data. We summarize recent results, primarily from the IUE satellite, which demonstrate the importance of time-dependent phenomena in hot-star outflows, and which, in particular, point to
