First Detection of Hard X-ray Emission From Solar Type III Radio Bursts

Details First Detection of Hard X-ray Emission From Solar Type III Radio Bursts First Detection of Hard X-ray Emission From Solar Type III Radio Bursts

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh11d1131c&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH11D-1131

Astronomy and Astrophysics

Astronomy

6954 Radio Astronomy, 6984 Waves In Plasma, 7504 Celestial Mechanics, 7531 Prominence Eruptions, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

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 Rsun) 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 ˜4, from the footpoint of a TRACE loop observed in FeXII (195 Å). Subsequently, jets are seen to originate from the RHESSI footpoint emission travelling with apparent speeds of ˜ 100 km s-1. The observed RHESSI hard X-ray fluxes require ˜1033 electrons above 10 keV. This work was supported by NASA contract NAS5-98033.

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