Na Deng Post-Doctoral Researcher

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Presentation transcript:

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

Rapid Penumbral Decay Associated with Flares NOAA 9026 2000/06/06 δ-Spot multi-polar X2.3 flare TRACE White-Light MDI Magnetogram

Intensity Evolution Area 1 & 2 intensity suddenly jumped to higher level  penumbral decay Area 3 intensity suddenly dropped to a lower level  umbral darkening.

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).

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

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.

Divergence Line of LCT Flow Field

Study of Stokes Profiles of Photospheric and Chromospheric Lines Present Work Study of Stokes Profiles of Photospheric and Chromospheric Lines Photosphere FeI 630.15 & 630.25 nm 100-250 km Low Chromosphere MgI b2 517.27 nm Temperature Minimum Region

Doppler Velocities Derived from Stokes I, V and LP Profiles

Stokes Inversion based on Response function (SIR) Photospheric FeI 630.15 & 630.25 nm Chromospheric MgI 517.27 nm

Comparison of Inverted Magnetic Field at Two Heights

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

Any suggestions are welcome 