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Stellar Outflows and Jets

Published online by Cambridge University Press:  25 April 2016

W. J. Zealey ,
R. Mundt ,
T. P. Ray ,
G. Sandell ,
T. Geballe ,
K. N. R. Taylor ,
P. M. Williams  and
H. Zinnecker
W. J. Zealey
Affiliation:
Department of Physics, University of Wollongong, Box 1144, Wollongong, N.S.W.2500, Australia
R. Mundt
Affiliation:
Max-Planck-Institute for Astronomy, Heidelberg, German Federal Republic
T. P. Ray
Affiliation:
School of Cosmic Physics, Dublin Institute of Advanced Studies, Dublin, Eire
G. Sandell
Affiliation:
Joint Astronomy Centre, Komohana Street, Hilo, Hawaii 96720, U.S.A.
T. Geballe
Affiliation:
Joint Astronomy Centre, Komohana Street, Hilo, Hawaii 96720, U.S.A.
K. N. R. Taylor
Affiliation:
Department of Physics, University of New South Wales, Kensington, N.S.W.2000, Australia
P. M. Williams
Affiliation:
Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, United Kingdon
H. Zinnecker
Affiliation:
Max Planck Institute of Physics and Astrophysics, Munich, German Federal Republic
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Abstract

We present maps in the visible emission lines of [S II] and the infrared emission lines of H2, at 2.12μm, for several bipolar outflow complexes which exhibit jet structures. A comparison of the morphology of this infrared emission and that seen in visible emission lines shows both the visible and the H2 emission exhibit clumpy structure on similar scales. It appears that the brightest H2 emission occurs at the working surfaces of the jets. Virtually no H2 emission is associated with the jets themselves.

Velocity profiles are presented for several objects and possible emission mechanisms are discussed.

Type
Stellar
Information
Publications of the Astronomical Society of Australia , Volume 8 , Issue 1 , 1989 , pp. 62 - 67
Copyright
Copyright © Astronomical Society of Australia 1989

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