Using HMI Data to Study Evolution of Solar Magnetic Fields and Predict Space Weather

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Using HMI Data to Study Evolution of Solar
Magnetic Fields and Predict Space Weather

• Haimin Wang
• Big Bear Solar Observatory
• New Jersey Institute of Technology

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Evolution of Magnetic Fields Associated with
Flares and CMEs

• Magnetic Fields
• Full Cadence
• Full Resolution
• Gradient Maps
• Shear Maps
• Extrapolated Coronal Field
• Flow Fields

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• Kosovichev and Zharkova, 2001, Ap.J. Letters, 550
  L105
• Changes of magnetic structure can take place in
  minutes, and in-reversible

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Before Flare After Flare
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01-04-06 X5.6 Flare
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Sudden Decay of Sunspot Penumbrae
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November 2, 2003 X8.3 Flare
before flare1650 UT after flare1830 UT
TRACE WL
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November 2, 2003 X8.3 Flare
RHESSI footpoints in 50-100 keV
aMDI magnetogram bTRACE WLcTRACE 1600 Å
dTRACE 195Å
Difference Image

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Time Profiles of
Mean Intensity and Magnetic Flux
D1 and D2penumbra decayingareas E1 and
E2corresponding umbra areas

• The penumbral fields turned more vertical but
  did not darken to become fully umbral fields.

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Explanation (3) Magnetic Reconnection
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Using HMI Data for Real Time Solar Activity
Forecasting

• Magnetic Gradient As Proxy of Magnetic Shear
• Vector Magnetogram from Huairou, Bastille Day
  flare on 2001-July-14

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Magnetic Gradient Vs. Magnetic Shear
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2001-4-6 2001-8-25
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2003-10-29 1991-6-9
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Field Extrapolation

• Linear Force-Free Field
• E.g., Yurchyshyn et al. 2001, Ap.J., 563, 381

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CME on July 14, 2000 Bastille Day Flare

• An erupted active regions magnetic field had WE
  orientation

and had the axial field directed east- wardly and
negative magnetic helicity. Since the loop had
southwardly directed azimuthal field, the
eruption caused a strong geomagnetic storm.
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Field Extrapolation

• Non-Linear Force Free Field
• E.g., Wheatland et al., 2000, Ap.J., 540, 1150

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Eveshed Flow
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• Shear Flow
• Yang et al. 2004, ApJL

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Detecting Sunspot Structure Below Surface

• Korukawa et al., 2002, Ap.J., 572, 598
• Compare to

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Small Scale Magnetic Fields

• Moving Magnetic Features
• Ellerman Bomb
• Network and IN Field
• Coronal heating
• Solar Wind

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Solar Wind Outflow and the Chromospheric Magnetic
Network Hassler et al., Science, 283, 810
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Key magnetograms with high sensitivity
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BBSOs Involvement in MHI

• Scientific research as discussed above. In
  addition we can contribute to the pipeline of
  data production
• 180 Ambiguity Solution (Moon et al., 2003, Solar
  Physics, 217, 79)
• Calibration of HMI Vector Magnetograms with our
  newly developed Near Infrared Imaging
  Magnetograph used in new 1.6 meter telescope
• Coronal Field Extrapolation combining MHI data
  with AIA data with artificial intelligence