Multi-Wavelength Observation Results of the C5.6 Limb Flare of 1 August 2003

Details Multi-Wavelength Observation Results of the C5.6 Limb Flare of 1 August 2003 Multi-Wavelength Observation Results of the C5.6 Limb Flare of 1 August 2003

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004soph..225...75l&link_type=abstract

Solar Physics, Volume 225, Issue 1, pp.75-90

Physics

5

Scientific paper

We obtained a complete set of Hα, Ca Π 8542 Å and He I 10830 Å spectra and slit-jaw Hα images of the C5.6 limb flare of 1 August 2003 using the Multi-channel Infrared Solar Spectrograph (MISS) at Purple Mountain Observatory. This flare was also observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and partially by the Extreme-ultraviolet Imaging Telescope (EIT) on SOHO. This flare underwent a rapid rising and expanding episode in the impulsive phase. All the Hα, Ca Π 8542 Å and He I 10830 Å profiles of the flare are rather wide and the widest profiles were observed in the middle bright part of the flare instead of at the flare loop top near the flare maximum. The flare manifested obvious rotation in the flare loop and the decrease of the rotation angular speed with time at the loop-top may imply a de-twisting process of the magnetic field. The significant increases of the Doppler widths of these lines in the impulsive phase reflect quick heating of the chromosphere, and rapid rising and expanding of the flare loop. The RHESSI observations give a thermal energy spectrum for this flare, and two thermal sources and no non-thermal source are found in the reconstructed RHESSI images. This presumably indicates that the energy transfer in this flare is mainly by heat conduction. The stronger thermal source is located near the solar limb with its position unchanged in the flare process and spatially coincident with the intense EUV and Hα emissions. The weaker one moved during the flare process and is located in the Hα dark cavities. This flare may support the theory of the magnetic reconnections in the lower solar atmosphere.

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