The C II infrared and ultraviolet lines

Details The C II infrared and ultraviolet lines The C II infrared and ultraviolet lines

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...134..193h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 134, no. 1, May 1984, p. 193-197.

Astronomy and Astrophysics

Astronomy

97

Carbon, Cosmochemistry, Infrared Astronomy, Ionic Collisions, Ultraviolet Astronomy, Chromosphere, Emissivity, Fine Structure, Interstellar Matter, Planetary Nebulae

Scientific paper

Effective collision strengths for C+ have been calculated for the fine structure transitions 2P01/2 - 2P03/2, and for transitions among the terms 2s22p2P0, 2s2p2 4P, 2D, 2S, 2P. The authors investigate the temperature and density dependence of relative emissivities of the multiplets λλ1335, 2325 under the assumption that excitation is due to collisions with free electrons. For the λ1335 multiplet the authors compare emissivities due to collisional excitation with those due to dielectronic recombination. Finally the cooling function for the infrared 158 μm transition is calculated.

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