標(biāo)題: Titlebook: Angular Momentum and Mass Loss for Hot Stars; L. A. Willson,R. Stalio Book 1990 Kluwer Academic Publishers 1990 Population.Variation.astro [打印本頁] 作者: 萬靈藥 時(shí)間: 2025-3-21 17:07
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書目名稱Angular Momentum and Mass Loss for Hot Stars讀者反饋
書目名稱Angular Momentum and Mass Loss for Hot Stars讀者反饋學(xué)科排名
作者: 用手捏 時(shí)間: 2025-3-21 20:55
Advances in Science, Technology & Innovationot show a tendency for the amplitudes to grow. Perhaps including time-dependent convection and/or modeling deeper envelopes with additional radiative damping will limit the pulsation amplitudes to observed values.作者: 終點(diǎn) 時(shí)間: 2025-3-22 00:42
Advances in Science, Technology & Innovationch may have a sequential evolutionary connection. For the Wolf Rayet stars the Luminous Magnetic Rotator model may be able to explain the long standing “wind momentum problem” as well as the “spin-down problem” associated with earlier rotating wind models. Constraints on the surface magnetic field a作者: Factorable 時(shí)間: 2025-3-22 07:07 作者: 外來 時(shí)間: 2025-3-22 09:38 作者: 裝飾 時(shí)間: 2025-3-22 13:34
Pulsation Studies of a 1.8 M⊙ Delta Scuti Modelot show a tendency for the amplitudes to grow. Perhaps including time-dependent convection and/or modeling deeper envelopes with additional radiative damping will limit the pulsation amplitudes to observed values.作者: 造反,叛亂 時(shí)間: 2025-3-22 20:55
Basic Magnetic Rotator Theory with Application to the Angular Momentum Driven Winds of B[e] and Wolfch may have a sequential evolutionary connection. For the Wolf Rayet stars the Luminous Magnetic Rotator model may be able to explain the long standing “wind momentum problem” as well as the “spin-down problem” associated with earlier rotating wind models. Constraints on the surface magnetic field a作者: 輕浮女 時(shí)間: 2025-3-23 01:04
Constraints on the Thickness of be Star Disks Derived from Combined IR Excess and Optical Polarimetron envelope, or by having partial cancellation of the equatorial polarization from contributions near the pole. The two solutions have different base densities, .., and may be differentiated by yet other observational data.作者: growth-factor 時(shí)間: 2025-3-23 05:00 作者: Conducive 時(shí)間: 2025-3-23 09:20 作者: 脫離 時(shí)間: 2025-3-23 11:47 作者: 沉著 時(shí)間: 2025-3-23 17:01 作者: 特別容易碎 時(shí)間: 2025-3-23 21:57
Evidence That Wolf-Rayet Stars are Pre-Main Sequence Objectsloud, and that their rate of mass loss is moderate. These properties are consistent with Wolf-Rayet stars being young objects recently arrived on the main sequence rather than the evolved, peeled-down remnants of massive stars.作者: 轉(zhuǎn)向 時(shí)間: 2025-3-23 23:57
A Statistical Study of Main Sequence A and F Stars: Testing the Main Sequence Mass Loss Hypothesis rotation has been suggested by Willson, Bowen, and Struck-Marcell (=WBS, 1987). These stars would evolve down the main sequence on a timescale that is less than or on the order of the nuclear evolution timescale. The mass loss process would end when the pulsation ends and/or when the rotation is braked.作者: 軌道 時(shí)間: 2025-3-24 03:45 作者: Shuttle 時(shí)間: 2025-3-24 08:17
Angular Momentum and Mass Loss for Hot Stars978-94-009-2105-4Series ISSN 1389-2185 作者: maverick 時(shí)間: 2025-3-24 11:55
https://doi.org/10.1007/978-3-642-28845-6“dynamical phenomena in stars and circumstellar envelopes”. Here I review the justification for the series and for the topic selected for this meeting, and note some relevant recent developments in our understanding of connections between angular momentum and mass loss for stars more massive than the Sun.作者: engrossed 時(shí)間: 2025-3-24 15:22 作者: Coronation 時(shí)間: 2025-3-24 22:22 作者: INTER 時(shí)間: 2025-3-25 02:39
https://doi.org/10.1007/978-3-030-01542-8 rotation has been suggested by Willson, Bowen, and Struck-Marcell (=WBS, 1987). These stars would evolve down the main sequence on a timescale that is less than or on the order of the nuclear evolution timescale. The mass loss process would end when the pulsation ends and/or when the rotation is braked.作者: 課程 時(shí)間: 2025-3-25 03:52
https://doi.org/10.1007/978-3-030-01542-8h, coordinated observations of variable stars. We also summarize the characteristics of the Santa Maria experiment which will be devoted to a long term, multiwavelength monitoring program of variable sources.作者: 噴出 時(shí)間: 2025-3-25 08:13
https://doi.org/10.1007/978-94-009-2105-4Population; Variation; astrophysics; interstellar matter; planet; star; stellar; stellar evolution; stellar 作者: 博愛家 時(shí)間: 2025-3-25 12:26 作者: Amorous 時(shí)間: 2025-3-25 18:09
Nato Science Series C:http://image.papertrans.cn/a/image/157525.jpg作者: 極小量 時(shí)間: 2025-3-25 22:03
https://doi.org/10.1007/978-3-642-28845-6“dynamical phenomena in stars and circumstellar envelopes”. Here I review the justification for the series and for the topic selected for this meeting, and note some relevant recent developments in our understanding of connections between angular momentum and mass loss for stars more massive than th作者: Handedness 時(shí)間: 2025-3-26 04:13
https://doi.org/10.1007/978-3-642-28845-6 core. Single stars and detached components in close binaries are considered in turn. (The effects of rotation are so strikingly different in single and double stars that they are worth discussing in the same review.) For single stars I summarize in nontechnical terms what is known about the interac作者: 新手 時(shí)間: 2025-3-26 04:44 作者: 違法事實(shí) 時(shí)間: 2025-3-26 09:08
Fire Ecology of the Recent Anthropocened arrival on the main sequence. The degree of angular momentum loss is a strong function of mass, with low mass stars (M<1.3M.) experiencing the most angular momentum loss. This angular momentum loss prevents the use of low mass main sequence stars in studies of primordial stellar angular momentum. 作者: LUDE 時(shí)間: 2025-3-26 13:11 作者: Cytokines 時(shí)間: 2025-3-26 19:46 作者: GRE 時(shí)間: 2025-3-27 00:49
https://doi.org/10.1007/b137853loud, and that their rate of mass loss is moderate. These properties are consistent with Wolf-Rayet stars being young objects recently arrived on the main sequence rather than the evolved, peeled-down remnants of massive stars.作者: 強(qiáng)化 時(shí)間: 2025-3-27 03:01 作者: Aggrandize 時(shí)間: 2025-3-27 05:18
Advances in Science, Technology & Innovationh rates of linear radial and non-radial pulsations. Comparisons with earlier partially-analytical calculations by Lee (1985) show good agreement. The radial modes of three 60-zone envelope models based on this same evolution model are also being studied using a nonlinear hydrodynamics code with time作者: 痛恨 時(shí)間: 2025-3-27 11:48 作者: Fibrinogen 時(shí)間: 2025-3-27 17:05
https://doi.org/10.1007/978-3-030-01542-8 rotation has been suggested by Willson, Bowen, and Struck-Marcell (=WBS, 1987). These stars would evolve down the main sequence on a timescale that is less than or on the order of the nuclear evolution timescale. The mass loss process would end when the pulsation ends and/or when the rotation is br作者: 諷刺 時(shí)間: 2025-3-27 21:20
Advances in Science, Technology & Innovationtic rotator and the extreme case of centrifugal magnetic rotator winds are explained. Special emphasis is given to the stellar properties which determine the energy deposition, mass loss rate, and the terminal wind speed. Magnetic rotator winds are always hybrid winds, in which there is a “primary” 作者: CAGE 時(shí)間: 2025-3-28 01:01 作者: HAWK 時(shí)間: 2025-3-28 06:10 作者: Parameter 時(shí)間: 2025-3-28 09:52
https://doi.org/10.1007/978-3-030-01542-8of viscous forces were included in the motion equations. The line radiation force is considered with the inclusion of the finite disk correction in self-consistent computations which also contains gravity darkening as well as distortion of the star by rotation..An application to a typical B1V star l作者: 一瞥 時(shí)間: 2025-3-28 14:27
Advances in Science, Technology & Innovation Since the features have nearly zero velocity, they are probably evidence of differences between the line spectra of polar and equatorial regions. Rotationally induced temperature and gravity gradients or polar spots are the simplest explanation at the moment; a reliable discrimination requires obse作者: 友好關(guān)系 時(shí)間: 2025-3-28 17:52 作者: 植物學(xué) 時(shí)間: 2025-3-28 20:58
https://doi.org/10.1007/978-3-030-01542-8 envelope by the stellar disk or depolarization effects due to the finite angular size of the stellar disk. It is assumed that the wind is isothermal and that the electron scattering optical depth is less than unity for all lines of sight. The model is applied to the data for four Be stars which hav作者: prodrome 時(shí)間: 2025-3-29 02:13
The Herbig Ae and Be Stars: Mass and Angular Momentum Losses relatively high mass loss and rotation rates of these stars provide a strong indication that angular momentum loss might play a major role in their evolution, and might even be the source for their paradoxical active phenomena.作者: 禁止,切斷 時(shí)間: 2025-3-29 04:51 作者: APEX 時(shí)間: 2025-3-29 07:37
Intensive Photometric Campaign on Be Stars: Behaviour of Short-Term Periodic Variations and Its Relathis case nearly all the light variation must be due to temperature variations and the model is observationally indistinguishable from the starspot model. We suggest that the localized areas responsible for the light variations are regions of enhanced mass loss.作者: CROAK 時(shí)間: 2025-3-29 13:36
1389-2185 and efficiency of the processes by which angular momentum is redistributed within and lost from stars, and the role that stellar rotation plays in enhancing or driving stellar mass loss. There appears to be a qualitative change in the nature and efficiency of these mechanisms near spectral type FO:作者: Monolithic 時(shí)間: 2025-3-29 19:37 作者: Complement 時(shí)間: 2025-3-29 20:21 作者: 公社 時(shí)間: 2025-3-30 01:57
Rotation, Pulsation and Atmospheric Phenomena in A—Type Starsulsation, and the possible presence of mass (and angular momentum) loss related to rapid rotation and/or pulsation in these stars. Moreover, some new results derived from the observations of the stars in the far IR are presented.作者: 遺留之物 時(shí)間: 2025-3-30 04:50 作者: omnibus 時(shí)間: 2025-3-30 08:31 作者: alliance 時(shí)間: 2025-3-30 16:03
Earth System Science in the Anthropocene relatively high mass loss and rotation rates of these stars provide a strong indication that angular momentum loss might play a major role in their evolution, and might even be the source for their paradoxical active phenomena.作者: 極端的正確性 時(shí)間: 2025-3-30 19:40 作者: 招致 時(shí)間: 2025-3-30 22:46 作者: 紋章 時(shí)間: 2025-3-31 04:07
https://doi.org/10.1007/978-3-642-28845-6their huge mass ejections is also discussed. Finally, a few possible evidences for rotationally or tidally induced mixing in massive O-stars are presented, suggesting that some very massive stars may evolve close to homogeneity.作者: CLAIM 時(shí)間: 2025-3-31 05:01 作者: ABOUT 時(shí)間: 2025-3-31 09:34
Advances in Science, Technology & Innovationsuch a wind model is constructed, and how it leads to a wind which is slow and dense in the equatorial regions and fast and tenuous along the poles. I will also describe the limitations of the model and observational evidence which cannot yet be explained by models of this type.作者: follicle 時(shí)間: 2025-3-31 15:07
Advances in Science, Technology & Innovation variations have a noticeable effect on observed line profiles only if the pole is not too far from the center of the visible stellar disk. Therefore, the phenomenon provides an easy-to-use criterion for the identification of (rapidly rotating) stars seen at small to intermediate inclination angles.作者: lacrimal-gland 時(shí)間: 2025-3-31 18:52 作者: 共同給與 時(shí)間: 2025-3-31 23:34 作者: 腫塊 時(shí)間: 2025-4-1 03:37
The Connection between Rotation and the Winds of Be Starssuch a wind model is constructed, and how it leads to a wind which is slow and dense in the equatorial regions and fast and tenuous along the poles. I will also describe the limitations of the model and observational evidence which cannot yet be explained by models of this type.作者: Aesthete 時(shí)間: 2025-4-1 07:48
