Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...165..163w&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 165, no. 1-2, Sept. 1986, p. 163-169.
Astronomy and Astrophysics
Astrophysics
14
Emission Spectra, Metallicity, Resonance Lines, Solar Spectra, Ultraviolet Spectra, Calcium, Iron, K Lines, Photosphere, Solar Atmosphere
Scientific paper
The emission line Fe II 3969.4 A seen on the solar disk in the wing of Ca II H is shown to be formed as a result of the effective excitation in the upper photosphere in the wings of resonance lines of multiplet UV1 by the photospheric UV photons. The absence of intense emission cores in the resonance lines and the observed intensity of 3969.4 A line can be explained if neutral hydrogen collisions are taken into account, reducing their cross-section by a factor of about five with respect to the estimate of Drawin (1968, 1969) and Steenbock and Holweger (1984). Collective effects of the UV1 resonance lines and the thermalization by neutral hydrogen collisions are essential for the formation of the Fe II line in the wing of Ca II H.
Steenbock W.
Watanabe Ta.
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