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Modeling Outflows from Young Stars

Published online by Cambridge University Press:  23 September 2016

Hsien Shang
Hsien Shang*
Affiliation:
Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan

Abstract

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We have constructed the foundations to a series of diagnostics methods to probe the jet phenomena in young stars as observed at various optical forbidden lines and radio wavelengths. We calculate and model in a self-consistent manner the physical and radiative processes, which arise within an inner disk-wind driven magnetocentrifugally from the circumstellar accretion disk of a sun-like star. Comparing with real data taken at high angular resolution, our approach will provide the basis of systematic diagnostics for jets and their related young stellar objects, to attest the emission mechanisms of such phenomena. Such approach can help bring first-principle theoretical predictions to confront actual multi-wavelength observations, and will bridge the link between complex numerical simulations and observational data. Analysis methods discussed here are immediately applicable to new high-resolution data obtained with HST, Adaptic Optics, and radio interferometry.

Information

Type
Part 7: Jets and Outflows
Information
Symposium - International Astronomical Union , Volume 221: Star Formation at High Angular Resolution , 2004, pp. 351 - 358
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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