Structure of Magnetocentrifugal Disk-Winds: From the Launching Surface to Large Distances
- Others:
- Alves, João F.
- McCaughrean, Mark J.
Abstract
Protostellar jets and winds are probably driven magnetocentrifugally from the surface of accretion disks close to the central stellar objects. The exact launching conditions on the disk, such as the distributions of magnetic flux and mass ejection rate, are poorly unknown. They could be constrained from observations at large distances, provided that a robust model is available to link the observable properties of the jets and winds at the large distances to the conditions at the base of the flow. We discuss the difficulties in constructing such large-scale wind models, and describe a novel technique which enables us to numerically follow the acceleration and propagation of the wind from the disk surface to arbitrarily large distances and the collimation of part of the wind into a dense, narrow "jet" around the rotation axis. Special attention is paid to the shape of the jet and its mass flux relative to that of the whole wind. The mass flux ratio is a measure of the jet formation efficiency.
Additional Information
© 2002 Springer-Verlag Berlin Heidelberg. First Online: 15 October 2003.Attached Files
Accepted Version - 0107315v1.pdf
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Additional details
- Eprint ID
- 96131
- Resolver ID
- CaltechAUTHORS:20190605-083753380
- Created
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2019-06-06Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
- Caltech groups
- TAPIR
- Series Name
- ESO Astrophysics Symposia