Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987afz....26..263e&link_type=abstract
(Astrofizika, vol. 26, Mar.-Apr. 1987, p. 263-274) Astrophysics (ISSN 0571-7132), vol. 26, no. 2, Sept. 1987, p. 162-169. Transl
Astronomy and Astrophysics
Astrophysics
3
Planetary Nebulae, Resonance Lines, Silicon, Stellar Spectra, Hydrogen Ions, Integral Equations, Ionization, Optical Thickness, Transition Probabilities
Scientific paper
The optical thicknesses are calculated for a group of ultraviolet pseudoresonance lines of Si III (lines for which the lower levels are metastable and which are formed in the nebula itself). For this purpose, the coefficients Aij of spontaneous transitions have been found for more than 100 transitions between all levels of the 12 lowest terms of Si III. Calculations to find the populations of these levels have been made for a model of a nebula for which the temperature of the nucleus (central star) is 100,000 K, the radius of the nucleus is 10-billion cm, the radius of the nebula is R = 1.2 x 10 to the 17th cm, the concentration of hydrogen atoms is 10,000/cu cm, and the thickness of the nebula is H = 10 to the 17th cm. The values calculated for optical thicknesses were found to be of order unity for the following pseudoresonance lines of Si III: 997, 1108, 1113, 1296, and 1303.
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