Evolution and State of the Local ISM

  • T. Schmutzler
  • D. Breitschwerdt
Conference paper
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUS, volume 171)


The most puzzling observations concerning the LISM (distance < 100 pc) can be explained by a fast adiabatically cooled gas in the cavity of an old superbubble. The ultrasoft X-ray background and contributions to the Cand M-bands are due to the continuum emission of delayed recombination [1]. In contrast to collisional ionization equilibrium (CIE) models, but consistent with recent observations [2], our model predicts a lack of emission lines and a low emissivity in the EUV range. In the figure below we compare the emissivities resulting from CIE at T = 106 K and those from our model at T = 4.2 × 104 K. The basic feature of our model is a thermally self-consistent approach of the time-dependent evolution.


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    Breitschwerdt, D., Schmutzler, T., 1994, Nature, 371, 774–777ADSCrossRefGoogle Scholar
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    Jelinsky, P., Vallerga, J.V., Edelstein, J., 1995, Astrophys. J., 442, 653–661ADSCrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1996

Authors and Affiliations

  • T. Schmutzler
    • 1
  • D. Breitschwerdt
    • 2
  1. 1.Institut für Theoretische AstrophysikHeidelbergGermany
  2. 2.Max-Planck-Institut für KernphysikHeidelbergGermany

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