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.

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.

continuum

-4He fusion lines

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?

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)

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

1/20/2005

10/28/2003

11/02/2003