Abstract
THE electron temperature of a planetary nebula can be determined from the relative intensities of the N 1 and N 2 lines of [OIII] at λλ5,007, 4,959, and the ‘auroral’ type transition at λ4,363, provided the target areas for collisional excitation are known1.
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References
See for example, Menzel, D. H., Aller, L. H., and Hebb, M. H., Astrophys. J., 93, 230 (1941). New values for the target areas have been calculated by Seaton, M. J., Proc. Roy. Soc., A, 218, 400 (1953).
MacRae, D. A., Astro. J., 58, 43 (1953).
Astrophys. J., 93, 236 (1941); 113, 125 (1951).
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MacRAE, D., STOCK, J. Photoelectric Spectrophotometry of Planetary Nebulæ. Nature 173, 589–590 (1954). https://doi.org/10.1038/173589b0
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DOI: https://doi.org/10.1038/173589b0
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