LINE OF SIGHT MAGNETIC FIELD EVOLUTION & 120310 DATA ANALYSIS

Dandan Ye

Content

Part 1 Line of Sight magnetic field evolution

Part 2 120310 SDO data analysis

Line of Sight magnetic field evolution

Paperview:

Flare Energy and Magnetic Field Variations

H. S. Hudson, G. H. Fisher, B. T. Welsch

Introduction: Magnetic field created in convection zone

and then ascends through the photosphere and emerges into the corona. The emerged flux contains embedded stresses that may accumulate for some period of time and then relax, producing a flare and/or a CME.

The photospheric vector magnetic field might vary across the duration of a solar flare or CME.

Line of Sight magnetic field evolution

Perhaps the first clear illustration of a flare-associated magneticfield change (Wang 1992)

Line of Sight magnetic field evolution

Simple model: to estimate the energy deposited in the subphotospheric layers in this back-reaction

Principle: any change of magnetic field energy must lead to a corresponding change in magnetic pressure

Line of Sight magnetic field evolution

Conclusion: They predict that flares can be

accompanied by rapid and irreversible changes of photospheric magnetic fields.

Line of Sight magnetic field evolution

OBSERVATIONAL EVIDENCE OF BACK REACTION ON THE SOLAR SURFACE ASSOCIATED WITH CORONAL MAGNETIC RESTRUCTURING IN SOLAR ERUPTIONS

Haimin Wang and Chang Liu

provides support for the theory and prediction of Hudson : photospheric magnetic fields must respond to coronal field restructuring and turn to a more horizontal state near the PIL after eruptions.

20120310 SDO data

20120310 SDO data

HMI magnetogram

AIA 171 304 1600

20120310 SDO data

20120310 SDO data

20120310 SDO data

20120310 SDO data

Next Steps

Analyzing the line-of-sight magnetic field evolution of the 20121023 X-class flare as a practice

Try to do a running average of flow-field data on 20120701

Doing some study about the flares on 20120310

Thanks!