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Theoretical models of interstellar shocks. I - Radiative transfer and UV precursorsTheoretical models of interstellar radiative shocks are constructed, with special attention to the transfer of ionizing radiation. These models are 'self-consistent' in the sense that the emergent ionizing radiation (the UV precursor) is coupled with the ionization state of H, He, and the metals in the preshock gas. For shock velocities of at least 110 km/s the shocks generate sufficient UV radiation for complete preionization of H and He, the latter to He(+). At lower velocities the preionization can be much smaller, with important consequences for the cooling function, the shock structure, and the emission. For models with shock velocities of 40 to 130 km/s the intensities of the strongest emission lines in the UV, optical, and infrared are tabulated, as well as postshock column densities of metal ions potentially observable by UV absorption spectroscopy. Possible applications to supernova remnants and high-velocity interstellar gas are assessed.
Document ID
19790036154
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Shull, J. M.
(California, University Berkeley, Calif.; Colorado, University; Joint Institute for Laboratory Astrophysics, Boulder, Colo., United States)
Mckee, C. F.
(California, University Berkeley, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
January 1, 1979
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
79A20167
Funding Number(s)
CONTRACT_GRANT: NGR-05-003-578
CONTRACT_GRANT: NSF AST-77-23069
CONTRACT_GRANT: NSF AST-75-23590
Distribution Limits
Public
Copyright
Other

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