Sigmoid, Type II Precursor, and Coronal Mass Ejection

Details Sigmoid, Type II Precursor, and Coronal Mass Ejection Sigmoid, Type II Precursor, and Coronal Mass Ejection

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0907l&link_type=abstract

American Astronomical Society, SPD meeting #37, #9.07; Bulletin of the American Astronomical Society, Vol. 38, p.236

Astronomy and Astrophysics

Astronomy

Scientific paper

The 2005 May 13 flare occurred in the sigmoidal active region, NOAA 10759, and its time dependent change on the TRACE, EIT, and SXI images suggests an eruption process as envisioned by the runaway tether-cutting model. However, the onset of the eruption in the low corona and the final explosion of the magnetic field in the high corona are not directly observable at these wavelengths and we infer them indirectly from the radio data obtained with the Owens Valley Solar Array (OVSA), Green Bank Solar Radio Burst Spectrometer (GBSRBS), PHOENIX-spectrograph of ETH Zurich, and the Potsdam-Tremsdorf Spectrograph. The Potsdam spectrograph shows a so-called Type II Precursor in the early phase of loop expansion, indicating a coronal shock formed near the flare site. The GBSRBS spectra show a type III burst followed by type II bursts in the maximum phase, which implies opening of field lines and strong shock formation in the high corona. Finally, the radio pulsations are detected on the OVSA and PHOENIX spectrographs, which we interpret as due to the magnetic loop oscillation as a dynamic response to the mass ejection. These radio data along with the EUV and X-ray images are used to infer the runaway tether-cutting process during this event in all coronal heights.This work is supported by NSF/SHINE grant ATM-0548952 and NSF grant AST-0307670 to NJIT.

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