Hostname: page-component-669899f699-g7b4s Total loading time: 0 Render date: 2025-04-27T20:30:36.793Z Has data issue: false hasContentIssue false
  • English
  • Français

X-Ray Spectroscopy of Supernova Remnants

Published online by Cambridge University Press:  12 April 2016

R. Petre
R. Petre*
Affiliation:
NASA/Goddard Space Flight Center, Code 660, Greenbelt, MD 20771, USA

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 spectroscopy can provide vital information about the progenitors and environments of supernova remnants. Plasma diagnostics and spectral modelling can be used to infer the energy of the remnant, the density and composition of the surrounding medium, and the degree of equilibrium in the shock heated gas. A new generation of X-ray spectrometers, the first of which was the Broad-Band X-Ray Telescope (BBXRT), has improved our ability to make precise measurements of X-ray line fluxes and energies. We summarize the results obtained from the BBXRT mission. These include a definitive measurement of the Fe K line centroid in the Tycho remnant, production of the first narrow-band X-ray maps (of Puppis A) and the first measurement of an electron-ion equipartition timescales in evolved remnants.

Type
Supernova Remnants
Information
International Astronomical Union Colloquium , Volume 145: Supernovae and Supernova Remnants , 1996 , pp. 357 - 368
Copyright
Copyright © Cambridge University Press 1996

References

Becker, R. H., et al. 1979, ApJL, 318, L73–6.Google Scholar
Becker, R. H., et al. 1980, ApJL, 318, L5–8.Google Scholar
Fahlman, G. G., & Gregory, P. C. 1981, Nature, 318, 202–4.Google Scholar
Gregory, P. C., & Fahlman, G. G. 1980, Nature, 318, 805–7.Google Scholar
Hamilton, A. J. S., Sarazin, C. L., & Chevalier, R. A., 1983, ApJS, 51, 115–48.Google Scholar
Hamilton, A. J. S., Sarazin, C. L. 1984, ApJ 318, 601–11.Google Scholar
Hamilton, A. J. S., Sarazin, C. L., & Szymkowiak, A. E. 1986a, ApJ, 318, 698–712.Google Scholar
Hamilton, A. J. S., Sarazin, C. L., & Szymkowiak, A. E. 1986b, ApJ, 318, 713–21.Google Scholar
Hwang, U., Hughes, J. P., Cañizares, C. R., & Markert, T. H. 1993, ApJ, 414, 219.Google Scholar
Itoh, H. 1979, Pub. Astr. Soc. Japan, 318, 813–27.Google Scholar
Lasker, B. M. 1978, ApJ, 318, 109–21.Google Scholar
Markert, T. H., Cañizares, C. R., Clark, G. W., & Winkler, P. F., 1983, ApJ, 318, 134–44.Google Scholar
Petre, R., Szymkowiak, A. E., Seward, F. D., & Willingale, R. 1988, ApJ, 318, 215–38.Google Scholar
Raymond, J. C. & Smith, B. W. 1977, ApJS, 318, 419–66.Google Scholar
Serlemitsos, P. et al., 1992, Frontiers of X-Ray Astronomy, ed. Tanaka, Y. and Koyama, K., pp. 221–231. Tokyo: Universal Academy Press.Google Scholar
Winkler, P. F., Cañizares, C. R., Clark, G. W., Markert, T. H., Kalata, K., & Schnopper, H. W. 1982, ApJL, 246, L27–32.Google Scholar