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The Radiation Transfer of Soft X-rays

Published online by Cambridge University Press:  12 April 2016

Jürgen Kerp  and
Jochen Pietz
Jürgen Kerp
Affiliation:
Radioastronomisches Institut der Universität Bonn Auf dem Hügel 71, D-53121 Bonn, Germany
Jochen Pietz
Affiliation:
Radioastronomisches Institut der Universität Bonn Auf dem Hügel 71, D-53121 Bonn, Germany

Abstract

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We discuss the link between the halo plasma temperature and the power-law spectral index of the extragalactic background radiation. This link is of strong influence for the derivation of the Galactic halo intensity distribution. In principal, we can distinguish between two combinations of Galactic halo plasma temperature and power-law slope. The first combination consists of a halo plasma of Thalo = 106 K and an E−2 approximation of the extragalactic background radiation. The second combination is Thalo = 106.2 K and an E−1.5. Both combinations are in agreement with recent observational results, thus it is not feasible to discriminate between both models on the basis of X-ray data available. But, the soft X-ray background intensity distribution in the ¼ keV and ¾ keV ROSAT energy bands differs significantly. The Thalo = 106 K and an E−2 allows a patchy ¼ keV intensity distribution while the Thalo = 106.2 K and an E−1.5 predicts a much smoother intensity variation since the hotter halo plasma accounts for a significant fraction of the ¾ keV background radiation.

Type
Part VI Distant Hot Gas, SXRB Fluctuations, Dust, Gamma-rays
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 337 - 340
Copyright
Copyright © Springer-Verlag 1998

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