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Back Reaction on the Photospheric Magnetic field in Solar Eruptions Dandan Ye.

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Presentation on theme: "Back Reaction on the Photospheric Magnetic field in Solar Eruptions Dandan Ye."— Presentation transcript:

1 Back Reaction on the Photospheric Magnetic field in Solar Eruptions Dandan Ye

2 Contents Paper review: 2005 J.J. Sudol and J.W. Harvey ‘Longitudinal magnetic field changes accompanying solar flares’ My work about flare-related magnetic field evolutions to the X1.8 flare on

3 Paper review Background: Re-examined the basic assumptions of flare theories: the photospheric magnetic field does not change significantly during flares Data:15 X-class solar flares Global Oscillation Network Group (GONG) magnetograms

4 Paper review

5 The time variation of the magnetic field that occurs during a flare can be characterized to first order with a step function. (Sudol&Harvey 2004) a, b, c, n, and t 0 are the free parameters

6 Paper review X8.3 flare Time variation plots for (10*10) pixels

7 Paper review Left: magnetic field image of a 10-min average Middle: dB map Right: B vs t (representative points for four hours)

8 Paper review

9 Comparison with flare emission GONG & TRACE

10 Paper review Discussion: Abrupt, significant, and permanent changes of the photospheric longitudinal magnetic field are ubiquitous features of X-class flares. Reasons: unclear (like flows compress the field; parts of the field shift horizontally; flux submerges out of sight…..)

11 Paper review Many of the field changes with penumbrae and the recent observations show that penumbrae weaken during flares Penumbral magnetic field more vertical So, the field lines are pulled or relax upward by the erupting flare.

12 My work AR (close to the west limb) Line-of sight component of magnetic field change Vector of magnetic field change Intensity Data

13 My work Data: Helioseismic and Magnetic Imager(HMI) data on board the SDO LOS: Magnetogram with a spatial resolution of ~1'' and a cadence of 45 seconds Vector: Vector magnetic field with a spatial resolution of ~1'' and a cadence of 12 min. Intensity: Continuum data with a cadence of 45 seconds

14 My work Intensity

15 My work Intensity Dif_image :24-3:12

16 My work Transformation of field vectors Bh represents the components of B in the directions parallel to the photosphere Br is the radial field component

17 My work

18 Vector

19 My work

20 LOS Dif_image :30-3:00

21 My work LOS

22 My work LOS

23 My work LOS

24 My work LOS

25 My work Summary: 1. Obviously the X1.8 flare produces abrupt and significant magnetic field structure change in intensity, vector field and LOS. 2. For this X1.8 flare, the diskward flux would decrease and the limbward flux would increase.

26 My work

27 3. Prove the speculation in Wang & Liu (2010): Field lines changing to more vertical state when the central region pressure is released after flares. 4. Prove the speculation in Sudol & Harvey (2005).

28 Thanks!


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