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Uv Spectra of Nebulae and Novae
Published online by Cambridge University Press: 12 April 2016
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Optical spectra of nebulae and novae are dominated by recombination lines of H I, Be I and He II and by forbidden lines, such as those of [0 III]. Their IR spectra show the fine-structure lines and continua due to dust. Most of the lines observed in the UV (say from 3000 to 1200 Å) are either due to resonance transitions (e.g. C IV 1549) or are of intercombination type (e.g. C III] 1908). Some elements do not have many lines in the optical - nitrogen gives only [N II] and there are no forbidden lines of ionized carbon - and for such elements much valuable information is provided by UV lines (e.g. N III], N IV], N V, C II], C III] and C IV). Carbon/oxygen abundance ratios deduced from combined UV and optical observations agree well with those deduced from IR continuum features (Seaton, 1983).
- Type
- Session 3. Non-Solar Astrophysics
- Information
- Copyright
- Copyright © Naval Research Laboratory 1984. Publication courtesy of the Naval Research Laboratory, Washington, DC.
References
Clegg, R.E.S., Seaton, M.J., Peimbert, M. and Torres-Peimbert, S., 1983. MN, 205, 417.Google Scholar
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