HR: 0830h
AN: SH11D-1131    [PDF]
TI: First Detection of Hard X-ray Emission From Solar Type III Radio Bursts
AU: * Christe, S
EM: schriste@ssl.berkeley.edu
AF: Physics Department, University of California, Berkeley, CA 94720-7300
AU: Krucker, S
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450
AU: Lin, R P
AF: Physics Department, University of California, Berkeley, CA 94720-7300
AU: Lin, R P
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450
AU: Arzner, K
AF: Paul Scherrer Institut, PSI, Villigen, 5232 Switzerland
AU: Benz, A O
AF: Institute of Astronomy, ETH Zentrum, Zurich, 8092 Switzerland
AB: We present the first detection of non-flare related hard X-ray emission from type III radio bursts as observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). During a period of 15 minutes on 19 July 2002 14:23-14:35 UT, the WAVES instrument on the Wind spacecraft observed interplanetary type III radio bursts approximately every 2 minutes and each was accompanied by a 12-15 keV X-ray brightening observed by RHESSI. The radio and X-rays fluxes were found to be strongly correlated. No flares were reported in the SEC solar event reports during this time and only the strongest brightening is associated with a detectable enhancement in the GOES levels (A3 above a B8 background). Phoenix-2, a ground-based radio spectrometer, observed each interplanetary type III to extend down to 300 MHz (0.1 R$_\odot$) The strongest type III was also accompagnied by a cluster of decimetric radio emission in the frequency range 1 to 2 GHz. A close correlation is found between X-ray fluxes and the decimetric fluxes. X-ray spectra show non-thermal emission (9-30 keV) with an electron spectral power-law index of $\sim$4, from the footpoint of a TRACE loop observed in FeXII (195 \AA). Subsequently, jets are seen to originate from the RHESSI footpoint emission travelling with apparent speeds of $\sim$ 100 km s$^{-1}$. The observed RHESSI hard X-ray fluxes require $\sim$10$^{33}$ electrons above 10 keV. This work was supported by NASA contract NAS5-98033.
UR: http://sprg.ssl.berkeley.edu/~schriste/july19/
DE: 6954 Radio astronomy
DE: 6984 Waves in plasma
DE: 7504 Celestial mechanics
DE: 7531 Prominence eruptions
DE: 7554 X rays, gamma rays, and neutrinos
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting