1. Flow and Magnetic Fields of Solar Active Regions in Photosphere and Chromosphere
Na Deng
Post-Doctoral Researcher
California State University Northridge (CSUN)
&
Visiting Researcher
Space Weather Research Lab, NJIT

2. Rapid Penumbral Decay Associated with Flares
NOAA /06/ δ-Spot multi-polar X2.3 flare
TRACE White-Light
MDI Magnetogram

3. Intensity Evolution
Area 1 & intensity suddenly jumped to higher level  penumbral decay Area intensity suddenly dropped to a lower level  umbral darkening.

4. Interpretation ── Magnetic Breakout Model
(Antiochos 1999)
X2.3 Flare ─ Filament Eruption ─ CME
Background is MDI magnetogram
Color lines represent magnetic field lines
After the flare, field lines open leading to filament eruption and CME.
Field lines in peripheral penumbra change from more inclined to more vertical, which is related to penumbral decay and umbral darkening (enhanced magnetic field).

5. Penumbral Shear Flows along Magnetic Neutral Lines
Active Region on 2003 October 29, X10 Flare
10486

7. Flow Field Evolution of a Decaying Sunspot
Disc Center (DC)
Bright penumbral grains and umbral dots move inward.
Dark features in the outer part of penumbra move outward.

8. Divergence Line of LCT Flow Field

9. Study of Stokes Profiles of Photospheric and Chromospheric Lines
Present Work
Study of Stokes Profiles of Photospheric and Chromospheric Lines
Photosphere FeI & nm km
Low Chromosphere MgI b nm Temperature Minimum Region

10. Doppler Velocities Derived from Stokes I, V and LP Profiles

11. Stokes Inversion based on Response function (SIR)
Photospheric FeI & nm
Chromospheric MgI nm

12. Comparison of Inverted Magnetic Field at Two Heights

13. Works In Planning
Use WFA to Derive Chromospheric Magnetic Field and Compare with SIR Inversion Result
The Relationship among Magnetic Field Configuration, Penumbral Width and Evershed Flow in Photosphere and Chromosphere

14. Any suggestions are welcome 