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RHESSI 2003 October 28 Time Histories

This study analyzes the time histories of fluxes following the peak nuclear/511 keV line flux in solar flares observed by RHESSI. The analysis suggests a hard spectrum and pion decay contribution to the observed emissions. Changes in the 511 keV line width may reflect changes in the solar atmosphere or accelerated particle populations.

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RHESSI 2003 October 28 Time Histories

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  1. RHESSI 2003 October 28 Time Histories Falling fluxes following the peak Nuclear/511 keV line flux delayed relative to bremsstrahlung Fit to 511 keV line flux indicates a hard spectrum, including contribution from pion decay Continuum below 511 keV line just after impulsive peak also suggests positrons from pion decay RHESSI observed emission >9 MeV emission consistent with pion emission (CORONAS-F observed gamma rays from neutral pion emission.) Change in 511 keV line width after 11:16 may reflect change in solar atmosphere and/or population of accelerated particles.

  2. continuum a-4He fusion lines Expanded view of annihilation line region during 1st 240s of October 28 flare revealing different components: annihilation line and continuum (believed to be Compton scattered photons) and the alpha-He fusion line complex.

  3. RHESSI 2003 November 2 time histories Fast rise and gradually falling fluxes following the peak Nuclear/511 keV line flux delayed relative to bremsstrahlung 511-keV flux decay appears too flat relative to the calculation shown by solid curve. Change in 511-keV line width after 17:26?

  4. Comparison of sub-mm time history for Nov. 2, 2003 flare and hard X-ray and gamma-ray emissions measured by RHESSI (Silva et al 2006)

  5. 1/20/2005 Spectra from three RHESSI flares revealing differing amounts of pion radiation inferred from 9-16 MeV emission. Coronas confirms pion emission in the October 28 and January 20 flares. No evidence for pion emission in November 2 flare 10/28/2003 11/02/2003

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