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High Velocity Flow Suggested by Wing Components of the Hα Line Profiles in the Selected Planetary Nebulae

Published online by Cambridge University Press:  26 May 2016

S. Tamura ,
M. Otsuka  and
A. Tajitsu
S. Tamura
Affiliation:
1 Astronomical Institute, Tohoku University, Sendai 980-8578, Japan
M. Otsuka
Affiliation:
1 Astronomical Institute, Tohoku University, Sendai 980-8578, Japan
A. Tajitsu
Affiliation:
2 National Astronomical Observatory, NAOJ, Okayama, 719-0232, Japan

Extract

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This is a short report on the study of internal motions of selected Planetary nebulae. We have studied this subject with both high (4 or 8 Å/mm) and intermediate (20 Å/mm) dispersion spectrographs. During the course of this work we noticed the existence of a high velocity gas flow distinct from the well known expanding gas, but with smaller velocities than stellar winds (Yadoumaru & Tamura 1994 on Abell 30; Otsuka & Tamura, 2001 on H 4-1). We present subsequent results obtained with the intermediate dispersion spectrograph about 10 selected planetary nebulae. The analyses were made by multiple Gaussian method on the emission line profiles of Hα. High velocity gas flows were recognized by a weak broad wing component.

Type
Part VII: Nebular Morphology and Dynamics
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 539 - 540
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

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