Flare-generated Type II Burst without Associated Coronal Mass Ejection

Details Flare-generated Type II Burst without Associated Coronal Mass Ejection Flare-generated Type II Burst without Associated Coronal Mass Ejection

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...746..152m&link_type=abstract

The Astrophysical Journal, Volume 746, Issue 2, article id. 152 (2012).

Astronomy and Astrophysics

Astronomy

Shock Waves, Sun: Corona, Sun: Coronal Mass Ejections: Cmes, Sun: Flares, Sun: Radio Radiation

Scientific paper

We present a study of the solar coronal shock wave on 2005 November 14 associated with the GOES M3.9 flare that occurred close to the east limb (S06° E60°). The shock signature, a type II radio burst, had an unusually high starting frequency of about 800 MHz, indicating that the shock was formed at a rather low height. The position of the radio source, the direction of the shock wave propagation, and the coronal electron density were estimated using Nançay Radioheliograph observations and the dynamic spectrum of the Green Bank Solar Radio Burst Spectrometer. The soft X-ray, Hα, and Reuven Ramaty High Energy Solar Spectroscopic Imager observations show that the flare was compact, very impulsive, and of a rather high density and temperature, indicating a strong and impulsive increase of pressure in a small flare loop. The close association of the shock wave initiation with the impulsive energy release suggests that the impulsive increase of the pressure in the flare was the source of the shock wave. This is supported by the fact that, contrary to the majority of events studied previously, no coronal mass ejection was detected in association with the shock wave, although the corresponding flare occurred close to the limb.

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