Hostname: page-component-848d4c4894-jbqgn Total loading time: 0 Render date: 2024-06-19T19:44:40.787Z Has data issue: false hasContentIssue false
  • English
  • Français

High Resolution X-ray Spectra of Supernova Remnants

Published online by Cambridge University Press:  04 August 2017

C. R. Canizares ,
P. F. Winkler ,
T. H. Markert  and
C. Berg
C. R. Canizares
Affiliation:
Department of Physics and Center for Space Research Massachusetts Institute of Technology Alfred P. Sloan Research Fellow
P. F. Winkler
Affiliation:
Department of Physics, Middlebury College
T. H. Markert
Affiliation:
Department of Physics and Center for Space Research Massachusetts Institute of Technology
C. Berg
Affiliation:
Department of Physics and Center for Space Research Massachusetts 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 review results obtained with the Focal Plane Crystal Spectrometer (FPCS) on the Einstein Observatory. Clear evidence is found for departures from ionization equilibrium in the interior of Puppis A. This comes from the observed weakness of the forbidden lines relative to the resonance lines for the He - like triplets of O VII and Ne IX. However, it is shown that this departure from equilibrium does not alter our conclusion, based on previous FPCS results, that O and Ne are overabundant relative to Fe. The spectrum of N132D shows strong O VIII emission and very weak Fe emission, suggesting an even greater O/Fe abundance enhancement than in Puppis A. In the Cygnus Loop, the O to Ne abundance ratio is approximately solar; we have no information about Fe. The O VII triplet shows clear evidence for departures from ionization equilibrium in the Cygnus Loop. The spectrum of Tycho's SNR contains lines from ionization stages of Fe XVII through Fe XXIII and XXIV, indicating that a wide range of ionization conditions are present. Cas A and Kepler's SNR show relatively less emission from the higher ionization stages. For Tycho, we measured the strength of the strong Si XIII lines, and we find that a many-fold overabundance of Si relative to Fe is required regardless of the equilibrium state of the emitting plasma (confirming the Solid State Spectrometer results). On a separate topic, the completed analysis of X-ray Doppler shifts in Cas A suggests that the emitting material is concentrated in a ring that is inclined to the line of sight and is expanding at ~5000 km s−1.

Type
II. Middle Aged and Older Supernova Remnants
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 205 - 211
Copyright
Copyright © Reidel 1983 

References

Becker, R.H., Boldt, E.A., Holt, S.S., Serlemitsos, P.J. and White, N.E. 1980, Ap. J. (Letters), 237, p. L77.CrossRefGoogle Scholar
Becker, R.H., Holt, S.S., Smith, B.W., White, N.E., Boldt, E.A. Mushotzky, R.F., and Serlemitsos, P.J. 1980, Ap. J. (Letters), 235, p. L5.CrossRefGoogle Scholar
Becker, R.H., Holt, S.S., Smith, B.W., White, N.E., Boldt, E.A. Mushotzky, R.F. and Serelemitsos, P.J. 1979, Ap. J. (Letters), 234, p. L73.CrossRefGoogle Scholar
Canizares, C.R. and Winkler, P.F. 1981, Ap. J. (Letters), 246, p. L33.CrossRefGoogle Scholar
Fabian, A.c, Willingale, R., Pye, J.P., Murray, S.S. and Fabbiano, G. 1980, M.N.R.A.S. 193, p. 175.CrossRefGoogle Scholar
Hamilton, A.J.S., Sarazin, C.L. and Chevalier, R.A. 1982, preprint.Google Scholar
Itoh, H. 1979, Publ. Astron. Soc. Japan, 31, 541.Google Scholar
Lasker, B.M. 1980, Ap. J. 237, p. 765.CrossRefGoogle Scholar
Lasker, B.M. 1978, Ap. J. 223, p. 109.CrossRefGoogle Scholar
Long, K.S., Helfand, D.J. and Grabelsky, D.A. 1981, Ap. J. 248, p. 925.CrossRefGoogle Scholar
Markert, T.H., Canizares, C.R., Clark, G.W. and Winkler, P.F. 1983, Ap. J. (in press).Google Scholar
McKenzie, D.L. and Landecker, P.B. 1982, Ap. J. 259, p. 372.CrossRefGoogle Scholar
McKenzie, D.L., Landecker, P.B., Broussard, R.M., Rugge, H.R., Young, R.M., Fledman, U. and Doschek, G.A. 1980, Ap. J. 241, p. 409.CrossRefGoogle Scholar
Petre, R., Canizares, C.R., Kriss, G.A. and Winkler, P.F. 1982, Ap. J. 258, p. 22.CrossRefGoogle Scholar
Pradhan, A. 1982, Ap. J. (submitted).Google Scholar
Raymond, J.C. and Smith, B.W. 1979, Private communication.Google Scholar
Raymond, J.C. and Smith, B.W. 1977, Ap. J. Suppl. 35, p. 419.CrossRefGoogle Scholar
Tuohy, I.R., Clark, D.H., and Burton, W.M. 1982, Ap. J. (Letters), 260, p. L65.CrossRefGoogle Scholar
van den Bergh, S. 1971, Ap. J. 165, p. 457.CrossRefGoogle Scholar
Weaver, T.A. and Woosley, S.E. 1980, Ann. N.Y. Acad. Sci., 336, 335.CrossRefGoogle Scholar
Winkler, P.F., Canizares, C.R., Clark, G.W., Markert, T.H., Kalata, K. and Schnopper, H.W. 1981a, Ap. J. (Letters) 246, p. L27.CrossRefGoogle Scholar
Winkler, P.F., Canizares, C.R., Clark, G.W., Markert, T.H., and Petre, R. 1981b, Ap. J. 245, p. 574.CrossRefGoogle Scholar
Winkler, P.F., Canizares, C.R., Markert, T.H. and Szymkowiak, A.E. 1982, in Supernovae: A Survey of Recent Research, Rees, M.J. and Stoneham, R.J., eds., (D. Reidel), 501.CrossRefGoogle Scholar