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Possible Contributions of Supernova Remnants to the Soft X-ray Diffuse Background (0.1 - 1 keV)

Published online by Cambridge University Press:  04 August 2017

W. T. Sanders ,
D. N. Burrows ,
D. McCammon  and
W. L. Kraushaar
W. T. Sanders
Affiliation:
Department of Physics, University of Wisconsin-Madison, Madison, Wis 53706 U.S.A.
D. N. Burrows
Affiliation:
Department of Physics, University of Wisconsin-Madison, Madison, Wis 53706 U.S.A.
D. McCammon
Affiliation:
Department of Physics, University of Wisconsin-Madison, Madison, Wis 53706 U.S.A.
W. L. Kraushaar
Affiliation:
Department of Physics, University of Wisconsin-Madison, Madison, Wis 53706 U.S.A.

Abstract

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Almost all of the B band (0.10–0.19 keV) and C band (0.15–0.28 keV) X-rays probably originate in a hot region surrounding the Sun, which Cox and Anderson have modeled as a supernova remnant. This same region may account for a significant fraction of the M band (0.5–1 keV) X-rays if the nonequilibrium models of Cox and Anderson are applicable. A population of distant SNR similar to the local region, with center-to-center spacing of about 300 pc, could provide enough galactic M band emission to fill in the dip in the count rate in the galactic plane that would otherwise be present due to absorption of both the extra-galactic power law flux and any large-scale-height stellar (or galactic halo) emission.

Type
IV. Old Supernova Remnants - Heating of the Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 361 - 365
Copyright
Copyright © Reidel 1983 

References

Cox, D. P. and Anderson, P. R.: 1982, Ap. J., 253, pp. 268–289.Google Scholar
McCammon, D., Burrows, D. N., Sanders, W. T., and Kraushaar, W. L.: 1983, Ap. J., submitted.Google Scholar
Sanders, W. T., Kraushaar, W. L., Nousek, J. A., and Fried, P. M.: 1977, Ap. J. (Letters), 217, pp. L87–L91.CrossRefGoogle Scholar
Nousek, J. A., Fried, P. M., Sanders, W. T., and Kraushaar, W. L.: 1982, Ap. J., 258, pp. 83–95.Google Scholar
Rosner, R., Avni, Y., Bookbinder, J., Giacconi, R., Colub, L., Harnden, F. R. Jr., Maxson, C. W., Topka, K., and Vaiana, G. S.: 1981, Ap. J. (Letters), 249, pp. L5–L9.CrossRefGoogle Scholar