Nuclear γ-ray line emission induced by energetic ions in solar flares and by galactic cosmic rays

• Published in: Journal of physics. Conference series Vol. 366; no. 1; pp. 12026 - 5
• Main Authors: Kiener, J, Tatischeff, V, Benhabiles-Mezhoud, H, Séréville, N de, Belhout, A
• Format: Journal Article
• Language: English
• Published: Bristol IOP Publishing 01.01.2012
• Subjects: Bremsstrahlung; Cosmic dust; Cosmic rays; Emission; Emission analysis; Galactic cosmic rays; Gamma emission; Gamma ray spectra; Heavy ions; Interstellar gas; Mathematical models; Nuclear interactions; Nuclear reactions; Nuclei (nuclear physics); Physics; Solar atmosphere; Solar flares
• ISSN: 1742-6596; 1742-6588; 1742-6596
• DOI: 10.1088/1742-6596/366/1/012026

The γ-ray spectra ol the strongest solar flares often show a broad and complex structure in the 0.1-10 MeV region sitting on a bremsstrahlung continuum. This structure is composed of several outstanding narrow lines and of thousands of unresolved narrow and broad lines forming a quasi-continuum. The major part of this emission is due to prompt deexcitation lines following nuclear interactions of accelerated light and heavy ions with the atomic nuclei composing the solar atmosphere. A similar emission is expected from interactions of galactic cosmic rays with the interstellar gas and dust. Experimental nuclear reaction studies coupled with extensive calculations have been done in the last one and a half decade at Orsay for the modelisation of this γ-ray emission. After a description of the nuclear reaction studies the analysis of one solar flare spectrum and predictions for the emission from the inner Galaxy will be presented.