HR: 1340h
AN: SH13A-0273    [Abstracts]
TI: Multi-wavelength Observations of an Arcade Flare on the Solar Limb
AU: * Mausda, S
EM: masuda@stelab.nagoya-u.ac.jp
AF: STEL, Nagoya University, Honohara 3-13, Toyokawa, 442-8507 Japan
AU: Akita, K
EM: kyo@utc.osaka-gu.ac.jp
AF: Osaka Gakuin University, Kishibe-Minami 2-36-1, Suita, 564-5811 Japan
AU: Watanabe, K
EM: kwatana@stelab.nagoya-u.ac.jp
AF: STEL, Nagoya University, Furo, Chikusa, Nagoya, 464-8601 Japan
AU: Nagashima, K
EM: kaorin@kwasan.kyoto-u.ac.jp
AF: Kwasan Observatory, Kyoto University, Ohmine 17, Kita Kazan, Yamashina, Kyoto, 607-8471 Japan
AU: Nishizuka, N
EM: nisizuka@kwasan.kyoto-u.ac.jp
AF: Kwasan Observatory, Kyoto University, Ohmine 17, Kita Kazan, Yamashina, Kyoto, 607-8471 Japan
AB: 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. By using also other data (Hα, EUV, and so forth), the characteristics of this flare are summarized as follows. (1) This flare is an arcade flare. However, one side of arcade footpoints is occulted by the limb. 2) A CME is observed with SOHO/LASCO about one hour after the flare start time and its speed is about 1600 km/s. (3) Nonthermal radio (17GHz and 34GHz) emissions are observed from the whole arcade system. Intense emission comes from lower region of this arcade. (4) 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. (5) Higher-energy (> 25 keV) hard X-rays are mainly emitted at the footpoint regions. In addition to that, a weaker compact hard X-ray source is located above the low-energy hard X-ray source. This compact coronal source does not show any significant motion during the flare rising phase. (6) The high-energy had X-ray coronal source has a softer (γ ~ 6.6) spectrum than that (γ ~ 4.8) of the footpoint source. (7) The time profiles of these two hard X-ray sources are a little different. The time profile of the footpoint source shows a spike structure. The coronal source doesn't show any short-time variation. The hard X-ray intensity of this source continuously increases during the rising phase. 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 flare.
DE: 7509 Corona
DE: 7519 Flares
DE: 7534 Radio emissions
DE: 7554 X-rays, gamma rays, and neutrinos
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005