Highly ionized atoms in cooling gas

Details Highly ionized atoms in cooling gas Highly ionized atoms in cooling gas

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...310l..27e&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 310, Nov. 1, 1986, p. L27-L30. NSF-supported resear

Astronomy and Astrophysics

Astrophysics

159

Astronomical Models, Cooling Flows (Astrophysics), Galactic Evolution, Gas Cooling, Intergalactic Media, Line Spectra, Ultraviolet Spectra, Galaxies, Gas Density, Isobars (Pressure), Isochoric Processes, Mathematical Models, Stellar Coronas, Stellar Luminosity

Scientific paper

The ionization of low density gas cooling from a high temperature was calculated. The evolution during the cooling is assumed to be isochoric, isobaric, or a combination of these cases. The calculations are used to predict the column densities and ultraviolet line luminosities of highly ionized atoms in cooling gas. In a model for cooling of a hot galactic corona, it is shown that the observed value of N(N V) can be produced in the cooling gas, while the predicted value of N(Si IV) falls short of the observed value by a factor of about 5. The same model predicts fluxes of ultraviolet emission lines that are a factor of 10 lower than the claimed detections of Feldman, Bruna, and Henry. Predictions are made for ultraviolet lines in cooling flows in early-type galaxies and clusters of galaxies. It is shown that the column densities of interest vary over a fairly narrow range, while the emission line luminosities are simply proportional to the mass inflow rate.

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