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Infrared Emission-Lines and the Stellar Temperature

Published online by Cambridge University Press:  07 August 2017

Sueli M. Viegas  and
Ruth Gruenwald
Sueli M. Viegas
Affiliation:
Instituto Astronômico e Geofísico - USP, Av. Miguel Stefano, 4200, 04301-002 SÃo Paulo, SP Brazil
Ruth Gruenwald
Affiliation:
Instituto Astronômico e Geofísico - USP, Av. Miguel Stefano, 4200, 04301-002 SÃo Paulo, SP Brazil

Extract

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Observations of near infrared emission-lines are becoming available and can be a powerful tool to improve our knowledge on planetary nebulae properties. For wavelengths in the range 1 to 5 μm, the emission-lines correspond to atomic transitions of high ionized species of heavy elements. In particular, the [Si VI] 1.96μm and [Si VII] 2.48μm lines have already been detected (Ashley and Hyland, 1988).

Type
II. Highlights on the Nuclei
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 89
Copyright
Copyright © Kluwer 1993 

References

Ashley, M.C.B. and Hyland, A.R. (1988), Ap. J. 331, 532 CrossRefGoogle Scholar
Gruenwald, R.B. and Viegas, S.M. (1992), Ap. J. Suppl. Ser. 78, 153 Google Scholar
Pottasch, S. (1984), “Planetary Nebulae” Google Scholar
Stasinska, G. and Tylenda, R. (1986) A.&A. 155,137 Google Scholar