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Star formation in X-ray cluster cooling flowsThe basic equations for X-ray cluster cooling flows, including the effects of star formation, are derived. It is confirmed that cooling flows are thermally unstable, and it is found that the fastest-growing linear perturbations in the flow are radial, comoving, and isobaric. A local approximation for the star formation rate is developed which allows analytic solutions to be found for both isobaric and gravity-dominated cooling flows. These solutions are used to show how star formation reduces the gas density, thereby lowering the cooling rate, which raises the gas temperature relative to the non-star-forming case. The analytic solutions are also used to estimate the spatial distribution of newly formed stars. It is found that star formation must proceed at a nearly maximal rate if isothermal mass profiles are to result.
Document ID
19870059538
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
White, Raymond E., III
(Virginia, University Charlottesville; Cambridge University, United Kingdom)
Sarazin, Craig L.
(Virginia, University Charlottesville; Joint Institute for Laboratory Astrophysics, Boulder, CO, United States)
Date Acquired
August 13, 2013
Publication Date
July 15, 1987
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 318
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
87A46812
Funding Number(s)
CONTRACT_GRANT: NSF AST-81-20260
CONTRACT_GRANT: NAGW-764
Distribution Limits
Public
Copyright
Other

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