Titlebook: Jets from Young Stars; Models and Constrain Jonathan Ferreira,Catherine Dougados,Emma Whelan Textbook 2007 Springer-Verlag Berlin Heidelber

Delirium

正常

過份好問

Jets from Young Stars: The Need for MHD Collimation and Acceleration Processesifugal ejection (combining magnetic self-collimation and magnetic acceleration) appears as the most effective mechanism able to reproduce the observed jet properties at all evolutionary phases. The jets would then be intimately linked to angular momentum extraction from the accreting disk and/or star.

Bmd955

Introduction to Magneto-Hydrodynamicssented in this lecture such as the tension effect, confinement, magnetic diffusivity, magnetic field freezing, Alfvén waves, magneto-sonic waves, reconnection. A celebrated phenomenon of MHD will not be introduced in this brief lecture, namely the dynamo effect.

火光在搖曳

Curmudgeon

我吃花盤旋

Jets from Young Stars: The Need for MHD Collimation and Acceleration Processess. Measurements of jet collimation and jet ejection-accretion efficiencies are reviewed and compared at various evolutionary stages (from protostars to optically revealed objects). It is then shown that they cannot satisfactorily be accounted for by purely hydrodynamical processes. MHD magneto-centr

ASTER

河潭

Gudgeon

Stellar Wind Models Analytical models and simulations suggest that the ejection start very early in the life of a low mass star from the edge of the disk. Then, the jet is progressively ejected from a more central part of the system composed by the star and its accretion disk. Once the disk itself evaporates, the jet