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Highly ionized atoms in cooling gasThe 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.
Document ID
19870035050
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Edgar, Richard J.
(Virginia Univ. Charlottesville, VA, United States)
Chevalier, Roger A.
(Virginia, University Charlottesville, United States)
Date Acquired
August 13, 2013
Publication Date
November 1, 1986
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters to the Editor
Volume: 310
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
87A22324
Funding Number(s)
CONTRACT_GRANT: NAGW-764
Distribution Limits
Public
Copyright
Other

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