Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-19T05:38:30.541Z Has data issue: false hasContentIssue false
  • English
  • Français

The High Energy X-ray Spectra of Supernova Remnants

Published online by Cambridge University Press:  04 August 2017

Steven H. Pravdo  and
John J. Nugent
Steven H. Pravdo
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology
John J. Nugent
Affiliation:
Downs Laboratory of Physics, California Institute of Technology

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the results of fitting an ionization nonequilibrium (NIE) model to the high energy (> 5 keV) X-ray spectra of the young supernova remnants Cas A and Tycho. As an additional constraint, we demand that the models simultaneously fit lower energy, higher resolution data. For Cas A, a single NIE component can not adequately reproduce the features for the entire X-ray spectrum because 1) the ionization structure of iron ions responsible for the K emission is inconsistent with that of the ions responsible for the lower energy lines, and 2) the flux of the highest energy X-rays is underestimated. The iron K line and the high energy continuum could arise from the same NIE component but the identification of this component with either the blast wave or the ejecta in the “standard” model is difficult. In Tycho, the high energy data rule out a class of models for the lower energy data which have too large a continuum contribution.

Type
I. Young Supernova Remnants
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 29 - 36
Copyright
Copyright © Reidel 1983 

References

Allen, C.W., 1973, Astrophysical Quantities (3d ed.; London: Athlone Press).Google Scholar
Becker, R.H., Holt, S.S., Smith, B.W., White, N.E., Boldt, E.A., Mushotzky, R.F., and Seflemitsos, P.J., 1979, Ap. J, (Letters), 234, p. L73.CrossRefGoogle Scholar
Becker, R.H., Holt, S.S., Smith, B.W., White, N.E., Boldt, E.A., Mushotzky, R.F., and Seflemitsos, P.J., 1980, Ap. J. (Letters), 235, p. L5.CrossRefGoogle Scholar
Chevalier, R.A., 1975, Ap. J., 200, p. 698.CrossRefGoogle Scholar
Davison, P.J.N., Culhane, J.L., and Mitchell, R.J., 1976, Ap. J. (Letters). 206, L37.CrossRefGoogle Scholar
Fireman, E.L., 1974, Ap. J., 187, p. 57.CrossRefGoogle Scholar
Hamilton, A.J.S., Sarazin, C.L., and Chevalier, R.A., 1982, preprint.Google Scholar
Mason, K.O., Pravdo, S.H., Charles, P.A., Smith, B.W., and Raymond, J.C., 1979, unpublished spectral analysis of Cas A. Google Scholar
Nugent, J.J., 1982, , .Google Scholar
Pravdo, S.H., and Smith, B.W., 1979, Ap. J. (Letters), 234, p. L195.CrossRefGoogle Scholar
Pravdo, S.H., Smith, B.W., Charles, P.A., and Tuohy, I.R., 1980, Ap. J. (Letters), 235, p. L9.CrossRefGoogle Scholar
Raymond, J.C., and Smith, B.W., 1977, Ap. J. (Suppl.), 35, p. 419.CrossRefGoogle Scholar
Shull, M., 1982, preprint.Google Scholar
Winkler, P.F., 1979, in Proc. HEAO Science Symp., eds, Dailey, C. and Johnson, W. (NASA CP-2113), p. 244.Google Scholar