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Relation Between Physical Environment and its Chemistry in Orion KL

Published online by Cambridge University Press:  04 August 2017

M. Ohishi ,
N. Kaifu ,
H. Suzuki ,
T. Miyaji  and
M. Morimoto
M. Ohishi
Affiliation:
Nobeyama Radio Observatory, Japan
N. Kaifu
Affiliation:
Nobeyama Radio Observatory, Japan
H. Suzuki
Affiliation:
Nobeyama Radio Observatory, Japan
T. Miyaji
Affiliation:
Nobeyama Radio Observatory, Japan
M. Morimoto
Affiliation:
Nobeyama Radio Observatory, Japan

Extract

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Orion KL is a famous high-mass star forming region, and many investigations have studied its dynamical aspects. But the chemical aspects of Orion KL are still veiled. In this paper, from chemical and physical analysis, we show that there are differences in the chemistry among many “velocity elements” in the core of Orion KL.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 146 - 149
Copyright
Copyright © Reidel 1987 

References

Hasegawa, T., Kaifu, N., Inatani, J., Morimoto, M., Chikada, Y., Hirabayashi, H., Iwashita, H., Morita, K., Tojo, A., and Akabane, K.: 1984, Astrophys. J. 283, 117.CrossRefGoogle Scholar
Irvine, W.M., Schloerb, F.P., Hjalmarson, Å., and Herbst, E.: 1984, in Protostars and Planets II, ed. Black, D. (University of Arizona Press).Google Scholar
Plambeck, R.L., Wright, M.C.H., Welch, W.J., Bieging, J.H., Band, B., Ho, P.T.P., and Vogel, S.N.: 1982, Astrophys. J. 259, 617.CrossRefGoogle Scholar