Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-12T17:38:56.967Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution and State of the Local ISM

Published online by Cambridge University Press:  25 May 2016

T. Schmutzler  and
D. Breitschwerdt
T. Schmutzler
Affiliation:
Institut für Theoretische Astrophysik, Im Neuenheimer Feld 561, D–69120 Heidelberg, Germany
D. Breitschwerdt
Affiliation:
Max-Planck-Institut für Kernphysik, Postfach 10 39 80, D–69029 Heidelberg, Germany

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.

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 C- and 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.

Type
Poster Papers
Information
Symposium - International Astronomical Union , Volume 171: New Light on Galaxy Evolution , 1996 , pp. 442
Copyright
Copyright © Kluwer 1996 

References

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