Hostname: page-component-8448b6f56d-qsmjn Total loading time: 0 Render date: 2024-04-23T14:26:57.176Z Has data issue: false hasContentIssue false
  • English
  • Français

Non-Equilibrium Ionization X-ray Emission from Supernova Remnants

Published online by Cambridge University Press:  04 August 2017

J. Michael Shull
J. Michael Shull*
Affiliation:
Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards, Boulder, Colorado 80309

Extract

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.

X-ray spectra of young supernova remnants (SNR's) are perhaps the most spectacular examples of hot, line-emitting astrophysical plasmas. Heated to temperatures of 1 to 10 keV and enriched with the heavy element products of stellar nucleosynthesis, the plasma inside these SNR's emits prodigiously in lines of 0, Ne, Mg, Si, S, Ar, Ca, and Fe. Theoretical models of this emission provide measures of the plasma temperature and density, elemental abundances, and the degree of approach to ionization equilibrium. Thus, astrophysicists are offered the opportunity to test their understanding of the supernova explosion, its interaction with the interstellar medium, and the nucleo-synthetic processes which enrich our galaxy with heavy elements.

Type
I. Young Supernova Remnants
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 99 - 107
Copyright
Copyright © Reidel 1983 

References

Becker, R.H., Holt, S.S., White, N.E., Boldt, E.A., Mushotzky, R.F., and Serlemitsos, P.J.: 1980a, Astrophys. J. (Letters) 235, p. L5.Google Scholar
Becker, R.H., Holt, S.S., White, N.E., Boldt, E.A., Mushotzky, R.F., and Serlemitsos, P.J.: 1980b, Astrophys. J. (Letters) 237, p. L77.Google Scholar
Chevalier, R.: 1982, Astrophys. J. 258, p. 790.Google Scholar
Gorenstein, E., Seward, F., and Tucker, W.: 1983, in IAU Symp. #101, this volume, p. 1.Google Scholar
Gronenschild, E.: 1979, , .Google Scholar
Gull, S.F.: 1975, Monthly Notices Roy. Astron. Soc. 161, p. 47.Google Scholar
Hamilton, A.J.S., Sarazin, C.L., and Chevalier, R.A.: 1983, Astrophys. J. Suppl., in press.Google Scholar
Itoh, H.: 1977, Pub. Astron. Soc. Japan 29, p. 813.Google Scholar
Itoh, H.: 1979, Pub. Astron. Soc. Japan 31, pp. 429 and 541.Google Scholar
McKee, C.F.: 1974, Astrophys. J. 188, p. 335.Google Scholar
Pradhan, A.K., Norcross, D.W., and Hummer, D.G.: 1981, Astrophys. J. 246, p. 1031.Google Scholar
Pradhan, A.K. and Shull, J.M.: 1981, Astrophys. J. 249, p. 821.Google Scholar
Pravdo, S.H., Smith, B.W., Charles, P.A., and Tuohy, I.R.: 1980, Astrophys. J. (Letters) 235, p. L9.Google Scholar
Raymond, J.C. and Smith, B.W.: 1977, Astrophys. J. Suppl. 35, p. 419.CrossRefGoogle Scholar
Sarazin, C.L., Hamilton, A.J.S., and Chevalier, R.A.: 1983, in IAU Symp. #101, this volume, p. 109.Google Scholar
Sedov, L.I.: 1959, Dimensional Methods in Mechanics (New York: Academic Press).Google Scholar
Shull, J.M.: 1981a, Astrophys. J. Suppl. 46, p. 27.Google Scholar
Shull, J.M.: 1981b, in Proc. Symp. on X-Ray Astronomy and Spectroscopy (Goddard Space Flight Center, Oct. 1981), NASA Tech. Memo. 83848, p. 107.Google Scholar
Shull, J.M.: 1982, Astrophys. J. 262, p. 308.Google Scholar
Szymkowiak, A.E., Shull, J.M., Hamilton, A.K.S., and Holt, S.S.: 1983, in preparation.Google Scholar
Taylor, G.I.: 1950, Proc. Roy. Soc. London A 201, p. 159.Google Scholar
Winkler, P.F., Canizares, C.R., Clark, G.W., Markert, T.H., Kalata, K., and Schnopper, H.W.: 1981, Astrophys. J. (Letters) 246, p. L27.CrossRefGoogle Scholar