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Titlebook: Angular Momentum Evolution of Young Stars; S. Catalano,J. R. Stauffer Book 1991 Springer Science+Business Media Dordrecht 1991 CCD.dynamic

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期刊全称Angular Momentum Evolution of Young Stars
影响因子2023S. Catalano,J. R. Stauffer
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学科分类Nato Science Series C:
图书封面Titlebook: Angular Momentum Evolution of Young Stars;  S. Catalano,J. R. Stauffer Book 1991 Springer Science+Business Media Dordrecht 1991 CCD.dynamic
影响因子This book reports the Proceedings of the NATO Advanced Research Workshop on "An­ gular Momentum Evolution of Young Stars" held from 17 to 21 September 1990 at Noto, Italy. The workshop had its immediate origin in a discussion about the availability of stel­ lar rotation data, that took place in 1987 at Viana do Castelo Portugal during the NATO meeting, Formation and Evolution of Low Mass Stars. We recognized that nearly 20 years had passed since the last meeting on stellar rotation and that significant progress in the observation of rotation rates in low mass stars had been made. During the last 20 years, new efficient instrumentation (CCD and photon counting de­ tectors and echelle spectrographs) and new analysis techniques (profile Fourier analysis) have allowed us to measure rotational velocities as low as 1-2 km/s and to reach low mass stars in young clusters. Even with these advances, rotational velocities of low mass stars would have remained challenging to determine if all single, low mass stars later than GO had rotational velocities of order or less than 10 km/sec. Evidence that this is not always the case was first provided by the photometric variability data obtained by
Pindex Book 1991
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Magnetic Activity and Rotationrefore, the various forms of magnetic activity manifestation are intimately connected with the internal structure and evolution of stars, hence with their age and rotation regime..The remarkable success achieved in understanding the general outline of magnetic activity requires, however, further obs
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Angular Momentum Effects in Star Formationis period, significant redistribution of angular momentum must occur in the star, as indicated by the substantial discrepancy between deduced angular momenta in star formation sites in the cores of molecular clouds and in the youngest optically visible stars. A major problem is the short time scale,
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Small—Scale Structure and Angular Momentum Transfer in Protostellar Environments eddies of the turbulent cascade. We compute the probability distribution of the stochastic force and angular momentum fields induced by these eddies, assuming that the density and velocity correlation functions can be described as power laws. We also show that a point mass moving faster than the ve
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