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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Studies in Soviet History and Societyfferential rotation and the relation of rotation to activity cycles. Finally, an observing program is outlined that could lead to significantly better understanding of angular momentum loss over the next few years.

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Hdl348

https://doi.org/10.1007/978-1-349-09629-9the same for all classes. While for the subgiants the discontinuity seems to be the result of a magnetic braking, for the giants, that one results from a division between objects of significantly different ages. For the most luminous classes, the discontinuity results from the short duration of the first-crossing phase.

lymphedema

International Political Economy Series appears as if intermediate mass stars are built via accretion of material from large (r ~ 300 AU), massive circumstellar disks (M ~ 1 M.) on timescales t < 1 Myr (for stars with M > 3 M.). The initial stellar angular momentum reflects a balance between the angular momentum added from accreting disk material, and that carried away by a wind.

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CROW

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The X-Ray Emission from Pms Stars in Taurus-Auriga, and the Relationship with Other Diagnostics of Abetween the X-ray luminosity and the H-alpha emission, expressed as the ratio between the H-alpha and 25-micron far-infrared luminosity, indicator of disk emission. We argue that this indicates a real inhibition of the wind emission in the most X-ray active T Tauri stars and we suggest a picture in which this phenomenon is likely to take place.

CBC471

Multifrequency Monitoring of RU Lupi: Observational Results and a Modelults and a first attempt of their interpretation. The various phenomena observed in RU Lupi can be explained in term of a disk accretion onto an young star with a moderately strong global magnetic field. The role of axial rotation is also discussed.

出處

Rotational Velocities of Stars in Open Clusters: The Time Dependence Revisitedence of stellar rotation. The shape of the Vsini distribution is an extremely sensitive function of the α index of the braking law (dV/dt = -AV.). The comparison of Hyades + Praesepe and Pleiades observations favours the value . = 2. The Vsini distributions could not be reproduced with . = 3, the value corresponding to the so-called t. law.

MORPH