Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh44a1733y&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH44A-1733
Physics
7507 Chromosphere, 7519 Flares, 7526 Magnetic Reconnection (2723, 7835)
Scientific paper
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.
Cheng Chung-Chieh
Yang Yadong
No associations
LandOfFree
Magnetic Reconnection Rate in X- and M-class Solar Flares does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Magnetic Reconnection Rate in X- and M-class Solar Flares, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic Reconnection Rate in X- and M-class Solar Flares will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1418725