Gamma-Ray Line Emission from Superbubbles in the Interstellar Medium: The Cygnus Region

Details Gamma-Ray Line Emission from Superbubbles in the Interstellar Medium: The Cygnus Region Gamma-Ray Line Emission from Superbubbles in the Interstellar Medium: The Cygnus Region

2001-06-07

arxiv.org/abs/astro-ph/0106125v1

Astronomy and Astrophysics

Astrophysics

5 pages, 3 figures, to appear in Proc. of Gamma-Ray Astrophysics 2001, to be published in AIP Conf. Proc. Series

Scientific paper

10.1063/1.1419456

The star forming process in the Milky Way is non-uniform in time and space. The scale of star forming regions ranges from groups within a few pc to large segments of spiral arms with linear dimension of order kpc. When many stars form in a relatively small volume over a short duration, a localized starburst ensues. The energetic impact of such a burst of star formation can severely affect the dynamic structure of the gaseous disk. Stellar winds and supernova explosions drive an expanding superbubble, whose size eventually exceeds the scale height of the disk and thus drives a disk-wind blowing metal enriched gas into the halo. We discuss the basic scenario of superbubble evolution, emphasizing the associated gamma-ray line signatures. In particular, we discuss nuclear line emission from 26Al and 60Fe in the Cygnus region.

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