Accelerated Particle Properties in Solar Flares from Gamma-Ray Line Observations

Journal Article · Mon Feb 26 00:00:00 EST 2007 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.2713525· OSTI ID:21056748

Kiener, J; Tatischeff, V ^[1]; Weidenspointner, G ^[2]; Gros, M ^[3]; Belhout, A ^[4]

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1. CSNSM, IN2P3-CNRS and Univ Paris-Sud, 91405 Campus Orsay (France)
2. Centre d'Etude Spatiale des Rayonnements, 9 av. du Colonel Roche, 31028 Toulouse (France)
3. DSM/DAPNIA/Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette (France)
4. USTHB, Faculte de Physique, BP 32, El Alia, 16111 Bab Ezzouar, Algiers (Algeria)

In solar flares with strong {gamma}-ray emission, several prominent narrow lines can usually be observed emerging from a broad structure in the several hundred keV to several MeV region. They are produced by interactions of energetic protons, 3He and {alpha}-particles with the most abundant isotopes in the solar atmosphere. The underlying continuum is due to electron and positron bremsstrahlung and to the superposition of broad lines from accelerated heavy ions as well as numerous narrow nuclear lines which are too weak to be resolved individually. The properties of the accelerated particles in the October 28, 2003 flare observed with the gamma-ray spectrometer SPI onboard INTEGRAL were deduced by comparison of prominent narrow line fluence ratios, the line shapes of the 4.4 MeV 12C and 6.1 MeV 16O lines and the total nuclear line emission in the framework of a thick target interaction model.

• OSTI ID: 21056748
• Journal Information: AIP Conference Proceedings, Vol. 891, Issue 1; Conference: 6. Symposium on nuclear physics, Tours (France), 5-8 Sep 2006; Other Information: DOI: 10.1063/1.2713525; (c) 2007 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
ALPHA REACTIONS
BREMSSTRAHLUNG
CARBON 12
COMPARATIVE EVALUATIONS
ELECTRONS
ELEMENT ABUNDANCE
GAMMA DETECTION
GAMMA SPECTROSCOPY
HEAVY ION REACTIONS
HEAVY IONS
HELIUM 3 REACTIONS
KEV RANGE
MEV RANGE
OXYGEN 16
PHOTON EMISSION
POSITRONS
PROTON REACTIONS
PROTONS
SOLAR ATMOSPHERE
SOLAR FLARES