Optical coronal emission lines from equilibrium and cooling plasmas

Details Optical coronal emission lines from equilibrium and cooling plasmas Optical coronal emission lines from equilibrium and cooling plasmas

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...364..561g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 364, Dec. 1, 1990, p. 561-567.

Physics

Atomic Physics

9

Atomic Physics, Gas Ionization, Interstellar Matter, Plasma Cooling, Supernova Remnants, Emission Spectra, Fine Structure, Gas Cooling, Ground State, Line Spectra, Visible Spectrum

Scientific paper

A calculation has been made of the emission from gas at temperature of about 10 to the 6th K due to optical coronal lines that result from fine structure transitions within the ground states of highly ionized atoms. These lines include the Forbidden Fe X 6374-A line, the Forbidden Fe XIV 5303-A line, and many other lines from stages of ionization of S, Ca, Fe, and Ni. The calculations are valid in the limit of very low density, and apply to the diffuse gas found in supernova remnants, the interstellar medium in galaxies, and intergalactic gas. It is found that the amount of optical coronal emission produced by a given amount of cooling gas is largely unaffected by changes in element abundances (provided the proportions of heavy elements remain the same).

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