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Yang et al. 2004, ApJ, 617, L151

Photospheric shear flows along the magnetic neutral line of Active Region 10486 prior to an X10 flare. Yang et al. 2004, ApJ, 617, L151. 太陽雑誌会　 2005.5.16. Active Region 10486. TRACE white light. X-class flares in Active Region 10486. Day Start Peak Class

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Yang et al. 2004, ApJ, 617, L151

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  1. Photospheric shear flows along the magnetic neutral line of Active Region 10486 prior to an X10 flare Yang et al. 2004, ApJ, 617, L151 太陽雑誌会　2005.5.16

  2. Active Region 10486 TRACE white light

  3. X-class flares in Active Region 10486 Day Start Peak Class 2003.10.23 8:19 8:35 X 5.4 23 19:50 20:04 X 1.1 26 5:57 6:54 X 1.2 28 9:51 11:10 X17.2 29 20:37 20:49 X10.0 11. 2 17:03 17:25 X 8.3 4 19:29 19:50 X28.0 and 20 M-class, 16 C-class flares

  4. TRACE 1600Å

  5. Rapid penumbral decay following the X-class flare Wand et al. 2004, ApJ, 601, L195

  6. MDI magnetogram

  7. Observation Dunn Solar Telescope (Sacramento Peak) 2003 October 29 15:28-17:28 Wavelength : 527nm, Bandpass : 52nm Spatial resolution : 0.”14 Temporal resolution : 1 min 16:59UT 20:44UT

  8. Temporal evolution of the flare ribbons 38 km/s in the weaker (left) and 19 km/s in the stronger (right) magnetic field regions Xu et al. 2004, ApJ, 607, L131

  9. Local NIR (1.56μm) intensity maxima (red) and HXR contours (blue) Xu et al. 2004, ApJ, 607, L131

  10. These strong flows with velocities of up to 1.6 km/s occur along both sides of the magnetic neutral line The magnetic neutral line splits some of the flow patches right in the middle These flows are in opposite directions on both sides of the magnetic neutral line These flows already starts well before (more than 2 hr) the flare Magnetic stress was built up because of these shear flows?

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