Other
Scientific paper
Feb 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasp..107..148k&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 107, no. 708, p. 148-151
Other
9
Electron Energy, Emission Spectra, Forbidden Transitions, Line Spectra, Oxygen Spectra, Planetary Nebulae, Visible Spectrum, Atomic Excitations, Electron Impact, Electron Transitions, Spectrographs
Scientific paper
Electron impact excitation rates for transitions in O I, calculated with the R-matrix code, are used to derive the electron-temperature sensitive emission-line ratio R = I(2s22p4 (1D) -2s22p4 1S/2s22p4 (3P)1,2-2s22p4 1D = I(5577 A)/I(6300+6365 A), for a range of electron temperatures Te = 5000-20 000 K) and densities (ne = 104 - 106/cu cm) applicable to planetary nebulae. Experimental values of R for a number of planetaries have been measured from high-resolution (approximately 0.6 A FWHM) spectra obtained with the Hamilton Echelle spectrograph on the 3-m telescope at the Lick Observatory. These measurements should be particularly reliable, as the sample of planetaries was restricted to those with large enough radial velocities for the nebular (O I) 5577 A emission to be red- or blue-shifted from the atmospheric airglow feature by a sufficient amount for the former to be reliably determined. Electron temperatures deduced from the observed values of R are generally in good agreement with those derived from Te-sensitive line ratios in other species, providing observational support for the accuracy of the atomic data adopted in the calculations.
Aller Lawrence H.
Brown Paul J. F.
Hyung Siek
Keenan Francis P.
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