The ion composition of cooling interstellar gas

Details The ion composition of cooling interstellar gas The ion composition of cooling interstellar gas

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pazh...10...35s&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 10, Jan. 1984, p. 35-41) Soviet Astronomy Letters (ISSN 0360-0327), vol. 10, Jan.-Feb.

Astronomy and Astrophysics

Astronomy

4

Gas Ionization, Gas Temperature, Interstellar Gas, Ion Concentration, Supernova Remnants, Cooling, Gas Composition, Nonequilibrium Ionization, Temperature Dependence

Scientific paper

It is shown that the ion composition of cooling interstellar gas may differ significantly from the equilibrium composition and thus the estimates of its temperature based on the comparison of observed densities of high-charged ions with the theoretical ones obtained in ionization equilibrium computations may be erroneous. It is suggested that the observed absorption lines of ions C IV, S IV, S VI, N V and O VI may be formed in relative cool (T ≥ 104.2K) old supernova remnants.

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