TY - JOUR
T1 - Hard X-ray observations of a jet and accelerated electrons in the corona
AU - Glesener, Lindsay
AU - Krucker, Säm
AU - Lin, R. P.
PY - 2012/7/20
Y1 - 2012/7/20
N2 - We report the first hard X-ray observation of a solar jet on the limb with flare footpoints occulted, so that faint emission from accelerated electrons in the corona can be studied in detail. In this event on 2003 August 21, RHESSI observed a double coronal hard X-ray source in the pre-impulsive phase at both thermal and nonthermal energies. In the impulsive phase, the first of two hard X-ray bursts consists of a single thermal/nonthermal source coinciding with the lower of the two earlier sources, and the second burst shows an additional nonthermal, elongated source, spatially and temporally coincident with the coronal jet. Analysis of the jet hard X-ray source shows that collisional losses by accelerated electrons can deposit enough energy to generate the jet. The hard X-ray time profile above 20keV matches that of the accompanying TypeIII and broadband gyrosynchrotron radio emission, indicating both accelerated electrons escaping outward along the jet path and electrons trapped in the flare loop. The double coronal hard X-ray source, the open field lines indicated by TypeIII bursts, and the presence of a small post-flare loop are consistent with significant electron acceleration in an interchange reconnection geometry.
AB - We report the first hard X-ray observation of a solar jet on the limb with flare footpoints occulted, so that faint emission from accelerated electrons in the corona can be studied in detail. In this event on 2003 August 21, RHESSI observed a double coronal hard X-ray source in the pre-impulsive phase at both thermal and nonthermal energies. In the impulsive phase, the first of two hard X-ray bursts consists of a single thermal/nonthermal source coinciding with the lower of the two earlier sources, and the second burst shows an additional nonthermal, elongated source, spatially and temporally coincident with the coronal jet. Analysis of the jet hard X-ray source shows that collisional losses by accelerated electrons can deposit enough energy to generate the jet. The hard X-ray time profile above 20keV matches that of the accompanying TypeIII and broadband gyrosynchrotron radio emission, indicating both accelerated electrons escaping outward along the jet path and electrons trapped in the flare loop. The double coronal hard X-ray source, the open field lines indicated by TypeIII bursts, and the presence of a small post-flare loop are consistent with significant electron acceleration in an interchange reconnection geometry.
KW - Sun: X-rays, gamma rays
KW - Sun: corona
KW - Sun: flares
KW - Sun: radio radiation
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U2 - 10.1088/0004-637X/754/1/9
DO - 10.1088/0004-637X/754/1/9
M3 - Article
AN - SCOPUS:84863518357
SN - 0004-637X
VL - 754
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 9
ER -