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Infrared Emission-Lines and the Stellar Temperature

Published online by Cambridge University Press:  07 August 2017

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
Copyright
Copyright © Kluwer 1993 

References

Ashley, M.C.B. and Hyland, A.R. (1988), Ap. J. 331, 532 CrossRefGoogle Scholar
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