Transcript 2003 Oct/Nov

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.
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.
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 submm 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