Flow and Magnetic Fields of Solar Flow and Magnetic Fields of Solar Active Regions in Photosphere and Active Regions in Photosphere and

Chromosphere Chromosphere

Na DengNa Deng

Post-Doctoral Researcher California State University Northridge (CSUN)

&Visiting Researcher

Space Weather Research Lab, NJIT

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TRACE White-LightTRACE White-Light MDI MagnetogramMDI Magnetogram

NOAA 9026 2000/06/06 δ-Spot multi-polar X2.3 flare

Rapid Penumbral Decay Associated with Flares

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

Intensity EvolutionIntensity Evolution

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Interpretation Interpretation ──── Magnetic Breakout Model Magnetic Breakout Model

X2.3 Flare ─ Filament Eruption ─ CMEBackground is MDI magnetogramColor lines represent magnetic field linesAfter 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).

(Antiochos 1999)

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Active Region 10486 on 2003 October 29Active Region 10486 on 2003 October 29, X10 Flare, X10 Flare

1048610486 1048610486

Penumbral Shear Flows along Magnetic Neutral LinesShear Flows along Magnetic Neutral Lines

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Disc Center (DC)

Bright penumbral grains and umbral dots move inward.

Dark features in the outer part of

penumbra move outward.

Flow Field Evolution of a Decaying SunspotFlow Field Evolution of a Decaying Sunspot

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Divergence Line of LCT Flow FieldDivergence Line of LCT Flow Field

Present Work

Study of Stokes Profiles of Photospheric and Chromospheric Lines

PhotosphereFeI 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

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Stokes InversionStokes Inversion

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

Use WFA to Derive Chromospheric Magnetic Field and Compare with SIR Inversion Result

Works In PlanningWorks In Planning

The Relationship among Magnetic Field Configuration, Penumbral Width and Evershed Flow in Photosphere and Chromosphere

Any suggestions are welcome