Gamma-ray lines from OB associations at Z=Zsolar and Z=2Zsolar

Details Gamma-ray lines from OB associations at Z=Zsolar and Z=2Zsolar Gamma-ray lines from OB associations at Z=Zsolar and Z=2Zsolar

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..410.1059p&link_type=abstract

The fourth compton symposium. AIP Conference Proceedings, Volume 410, pp. 1059-1063 (1997).

Computer Science

Associations Of Stars In The Milky Way, Molecular Clouds, H2 Clouds, Dense Clouds, And Dark Clouds, Mass Loss And Stellar Winds, Gamma-Ray Sources, Gamma-Ray Bursts, Gamma-Ray

Scientific paper

We calculate the gamma-ray line emission induced by energetic particles (EPs) in molecular clouds coupled with OB associations, assuming that the EPs originate from the winds of massive stars. Their composition reflects the average wind composition of an individual Wolf-Rayet star or of a whole OB association. We consider two initial stellar metallicities (solar and twice solar), and show that the corresponding gamma-ray line ratios are different, and that the lines are narrower at twice solar metallicity, which is relevant to the inner Galaxy. Addressing the Orion emission detected by COMPTEL, we show that our average wind compositions satisfy the available constraints. We analyse the most relevant present and future observables (broad band ratios, 12C and 16O line widths, 12C*/16O* line ratio) and discuss the differences between our results and those obtained with a WC composition based only on the extreme late phase wind, as used up to now. In particular, we predict a flux of 1-210-5 ph cm-2 s-1 at ~0.450 MeV from the Orion complex, due to the de-excitation of the fusion-spallation products 7Li and 7Be. Such a flux is below the current OSSE upper limit, but above the expected sensitivity of INTEGRAL.

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