HR: 1340h
AN: SH13A-0271    [Abstracts]
TI: Marnetic and Energy Characteristics in Two-Ribbon X-Class Flares
AU: * Yang, Y
EM: elleysun@hotmail.com
AF: Institute of Space Science, National Central University, Jhongli, 320 Taiwan
AU: * Yang, Y
EM: elleysun@hotmail.com
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720 United States
AU: Ip, W
EM: wingip@astro.ncu.edu.tw
AF: Institute of Space Science, National Central University, Jhongli, 320 Taiwan
AU: Ip, W
EM: wingip@astro.ncu.edu.tw
AF: Graduate Institute of Astronomy, National Central University, Jhongli, 320 Taiwan
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720 United States
AU: Lin, R
EM: boblin@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, CA 94720 United States
AU: Lin, R
EM: boblin@ssl.berkeley.edu
AF: Department of Physics, University of California, Berkeley, CA 94720 United States
AB: Several two-ribbon X-class flares which occurred near the solar disk center are investigated in this study. Some specific sub-regions within an active region are selected to estimate the change in magnetic flux from pre-flare to post-flare states. The high-cadence (1-min averaged) MDI magnetogram provides comprehensive photospheric magnetic measurement during these flares. The extreme ultraviolet observations in the wavelengths of 171, 195, and 1600 nm obtained by TRACE are used to search for the correlation of magnetic changes in the corona and transition region. We also used the RHESSI data to identify the hard X-ray source regions and compare them with the magnetic observations. We found that the magnetic fluxes within or in the vicinity of ribbons can change permanently after a flare eruption. Transient magnetic changes are also found in sub-regions. The characteristics of these X-class flares will be discussed in detail in this presentation.
DE: 7519 Flares
DE: 7524 Magnetic fields
DE: 7554 X-rays, gamma rays, and neutrinos
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005