1. Magnetic Configuration and Non-potentiality of NOAA AR10486
Jin-ping Dun
（金平 敦）
Kwasan and Hida Observatories, Kyoto University

2. 1. Introduction NOAA 10486 Time: 23 October – 4 November ,2003
Location: S17,L283
Activities: 7X,16M,28C-class

3. The X-class Flares Date Time (UT) Event 23 (Oct.) 08:19 X5.4
02(Nov.) : X8.3
: X28

4. 2. Observation SOHO White Light Image SOHO MDI Magnetogram
TRACE 1600 Å　Image
Huairou Vector Magnetogram

5. ３. Some Physical Parameters
３.1 Magnetic　Shear Angle
３.2 Vertical Current
３.3 Current Helicity

6. ３.1 Magnetic Shear Angle Weighted Magnetic Shear Angle
Where and are the azimuth of the ith pixel of observed and potential transverse field respectively. And n is the sum of the pixels in the selected region. Bti is the transverse field strength of the ith pixel.
The potential field configuration was computed using the observed longitudinal field as a boundary condition.

7. ３.2 Vertical Current

8. ３.3 Vertical Current Helicity

9. 4. 1 The X17 Flare on 28th:

10. TRACE 1600 Å Images

11. 4. 2 The X10 Flare on 29th:

12. TRACE 1600 Å Images

13. 4.3 Selected Local Regions:
Initial Bright Regions
Maximum Phase Regions

14. 4.3 Selected Local Regions:

15. 5. Daily Evolution of Some Physical Parameters of the Selected Regions:
5.1 Magnetic　Shear Angle
5.2 Vertical Current
5.3 Current Helicity

16. 6. Conclusion
1) The initial bright regions of X18 flare on 28 developed strong magnetic shear angle, high vertical current and current helicity density.
2) The extended regions during the maximum phase of those two large X-class flares correspond to strong magnetic shear angle, high vertical current and current helicity density.
3) The initial bright region which corresponding the center part of the expanding regions during the maximum of the flare developed strong magnetic shear before the flare and still kept strong magnetic shear after the flare.
4）The magnetic shear of the initial bright region which did not corresponding the center part of the expanding regions during the maximum of the flare developed to strong before the flare and became weak after the flare. The vertical current and current helicity in such region also have such tendency.

17. Thank You！

18. SOHO White Light Image (10.28 00:00 UT)

19. SOHO MDI Magnetogram (10.28 0:0 UT)