Hard X-ray and radio observations of an arcade-type flare on the solar limb

Satoshi Masuda (1), Kyo Akita (2), Kyoko Watanabe (1), Kaori Nagashima (3), Naoto Nishizuka (3)

(1)STEL, Nagoya University
(2)Osaka Gakuin University
(3)Kwasan Observatory, Kyoto University

In order to investigate vertical structure of solar flares, especially vertical distribution of high-energy electrons and super-hot plasmas, we analyzed an M-class flare which occurred just on the west solar limb on June 2, 2003. The rising phase of this flare was well observed with Nobeyama Radio Heliograph and RHESSI. Nonthermal radio emissions are observed from the whole arcade system. Intense emission comes from lower region of this arcade. On the other hand, low-energy (~10 keV) hard X-ray emission, probably super-hot thermal emission, is located along the ridge of the arcade. Higher-energy (> 25 keV) hard X-rays are mainly emitted at the footpoint regions. A weaker compact hard X-ray source is also observed above the low-energy hard X-ray source. The high-energy had X-ray coronal source has a softer spectrum than that of the footpoint source. Integrating these multi-wavelength observational results, we try to reveal the behavior of the high-energy electrons and the evolution of the super-hot plasma in this arcade-type flare.

Correspondence

Satoshi Masuda(masuda@stelab.nagoya-u.ac.jp), STEL, Nagoya University

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