HR: 1340h
AN: SH44A-1733    [Abstracts]
TI: Magnetic Reconnection Rate in X- and M-class Solar Flares
AU: * Yang, Y
EM: yhyang@pssc.ncku.edu.tw
AF: Plasma and Space Science Center, National Cheng Kung University, Tainan, 70101, Taiwan
AU: Cheng, C
EM: frankcheng@pssc.ncku.edu.tw
AF: Plasma and Space Science Center, National Cheng Kung University, Tainan, 70101, Taiwan
AB: The magnetic reconnection is generally believed to be responsible for the energy release and particle acceleration in solar flares. Since the magnetic reconnection is difficult to be observed directly, the apparent motions of associated hard X-ray (HXR) kernels or H-alpha ribbons can be regarded as the chromospheric signatures of magnetic reconnection process and thus provides an important way to measure the magnetic reconnection rate in the corona. By combining the MDI (Michelson Doppler Imager) magnetograms, the reconstructed HXR images from RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Image), the H-alpha images from global high-resolution H£\ network, and the TRACE 160 nm images, the reconnection electric field and magnetic flux change rate in X- and M-class flares can be estimated. We will compare the results of magnetic reconnection rate from different measurements (HXR, H-alpha, EUV/UV). Comparison of reconnection rate between observation and theory will also be discussed.
DE: 7507 Chromosphere
DE: 7519 Flares
DE: 7526 Magnetic reconnection (2723, 7835)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting