Solar energetic particle events investigated with combined SOHO/COSTEP and Nancay radioheliograph observations

Details Solar energetic particle events investigated with combined SOHO/COSTEP and Nancay radioheliograph observations Solar energetic particle events investigated with combined SOHO/COSTEP and Nancay radioheliograph observations

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....5947p&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #5947

Computer Science

Scientific paper

It has long been known (cf. Kahler 1982, ApJ 261, 710) that solar energetic particle events are associated with complex radio emissions called type IV bursts. More recently, Cane et al. (2003, JGR, in press) established a close association between particle events at energies > 20 MeV with the radio emission from electron beams travelling through the corona at heights greater than ~2 Rs above the photosphere. These emissions occur together with coronal mass ejections. While statistical associations of particle events with various dynamic phenomena in the middle corona therefore seem to be well established, the detailed timing of the proton injection with respect to radio bursts and mass ejections has rarely been analysed. In this contribution, we combine particle data form SOHO/COSTEP with imaging and spectral observations at radio wavelengths in an attempt to constrain more closely the coronal processes that occur when the particle release starts at the Sun. For a set of eight well observed events the starting time of the proton injection is evaluated within an uncertainty of 10-30 minutes, and radio images of the corona are searched for simultaneous activity. In most cases broadband emission of duration > 10 min is found, pointing to sites of electron acceleration at heights below 1 solar radius above the photosphere. We discuss the timing of the proton release with respect to these emissions, to the CME and to radio signatures of shock waves and electron beams in the overlying corona.

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