Using Solar Gamma Rays to Measure Heavy Accelerated Particles at the Sun

Details Using Solar Gamma Rays to Measure Heavy Accelerated Particles at the Sun Using Solar Gamma Rays to Measure Heavy Accelerated Particles at the Sun

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh51c..05s&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH51C-05

Physics

Nuclear Physics

2716 Energetic Particles: Precipitating, 2720 Energetic Particles: Trapped, 7514 Energetic Particles (2114), 7519 Flares, 7554 X-Rays, Gamma Rays, And Neutrinos

Scientific paper

Solar flare gamma-ray spectra contain information on heavy (>He) accelerated particle spectra and composition through measurement of highly Doppler broadened (~10%) lines. These gamma-rays are emitted when the nuclei de-excite following their interaction with chromospheric H and He; these are called inverse reactions in contrast to the direct reactions from accelerated p and α-particles that produce narrower lines. The ability to distinguish and measure the broadened features is complicated by their large number, the narrow lines, the presence of strong solar bremsstrahlung and nuclear continua, as well as by instrumental effects. The instrumental continuum from Compton scattering is minimized when the gamma-ray detector has a high photopeak efficiency and is relatively well shielded, as was the case for the Solar Maximum Mission spectrometer (GRS). It is also important that the detector response be well determined. We have constructed a new GRS response matrix based on a Monte Carlo calculation and apply it to spectra from strong nuclear-line flares. We use new theoretical gamma-ray templates derived from nuclear physics calculations for elements such as C, O, Ne, Mg, Si, and Fe to fit the spectra and derive information on the heavy-accelerated ions. This technique can also be applied to data from the RHESSI spectrometer, with its larger Compton continuum, if the instrument response is well determined. This work was supported under NASA Grants NNX07AH81G, NNX07AO74G, and NNG06GG14G.

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