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
presentation
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