Possible origin of the diffuse Galactic 6.7 keV iron line, 511 keV annihilation line and of 1809 keV AL26 line

Details Possible origin of the diffuse Galactic 6.7 keV iron line, 511 keV annihilation line and of 1809 keV AL26 line Possible origin of the diffuse Galactic 6.7 keV iron line, 511 keV annihilation line and of 1809 keV AL26 line

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991aipc..232..155c&link_type=abstract

IN: Gamma-ray line astrophysics; Proceedings of the International Symposium, Paris, France, Dec. 10-13, 1990 (A92-43619 18-90).

Astronomy and Astrophysics

Astrophysics

Aluminum 26, Annihilation Reactions, Diffuse Radiation, Galactic Radiation, Iron, Line Spectra, Metallicity, Radioactive Isotopes, Stellar Mass Ejection, Supernova Remnants

Scientific paper

A recent measurement of the distribution of the 6.7 keV iron line flux along the galactic plane gives the opportunity to compare a model with the experimental results. The model is based on the assumption that supernova ejecta are responsible for the excitation of the interstellar iron and thus for the 6.7 keV iron line. The current supernova remnant distribution and a recent metallicity gradient were used. The result of the computation is well correlated with the observed iron flux versus the galactic longitude. The supernovae are progenitors of radioactive nuclei, some of which can decay via Beta(+) emission, for example Co-56, Ti-44, and Al-26. The Galactic source of 511 keV observed in the direction of the Galactic center are from two different origins: a steady diffuse component and a variable point source at/or near the Galactic center. The diffuse source of 511 keV is considered. The 1809 keV gamma-ray line was discovered in 1982 and confirmed. Possible distributions for both 511 keV and 1809 keV galactic lines which seem to fit the data quite well are proposed.

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