Investigation of the Acceleration Sites for Types II and III Radio Bursts during Solar Eruptions

Details Investigation of the Acceleration Sites for Types II and III Radio Bursts during Solar Eruptions Investigation of the Acceleration Sites for Types II and III Radio Bursts during Solar Eruptions

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh23b..02l&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH23B-02

Other

7513 Coronal Mass Ejections, 7519 Flares, 7524 Magnetic Fields, 7531 Prominence Eruptions, 7534 Radio Emissions

Scientific paper

Energetic properties of fast coronal mass ejections (CMEs) and the correlation of CMEs with flares suggest the production of high energy particles and CME-driven fast shocks in major solar eruptive processes. It is generally believed that the high energy particles, especially the energetic electron beams, are responsible for type III radio bursts, and that CME-driven shocks produce type II radio bursts. Observations show that type II bursts do not appear below a certain height. On the other hand, type III burst may be observed at both high and low altitudes. This indicates that acceleration sites of the electron beams may exist at both the CME-driven shock surface and the current sheet in the wake of CME, according to the catastrophe model of CMEs. The former could account for type III bursts at higher altitudes and the latter for those at lower altitudes. Both observations and theory show that the main acceleration phase of CMEs occurs in the lower corona, where the local Alfven speed (or the magnetosonic speed) is large, so that the CME-driven shocks may not develop until the CME reaches higher altitudes. On the basis of the catastrophe model of CMEs, we estimate that the highest frequency of type II burst is around 300 MHz, which corresponds to an altitude of ˜ 1.5× 105 km. This result is consistent with similar estimates based on observations that bring the corresponding frequency to a few hundred MHz.

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