Magnetic Shear in Two-ribbon Solar Flares Yingna Su 1,2 Advisors: Leon Golub 1, Guangli Huang 2...
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Magnetic Shear in Magnetic Shear in Two-ribbon Solar FlaresTwo-ribbon Solar Flares
Yingna SuYingna Su1,21,2
Advisors: Leon GolubAdvisors: Leon Golub11, Guangli Huang, Guangli Huang22
Collaborators: A. A. Van BallegooijenCollaborators: A. A. Van Ballegooijen11, E. E. Deluca, E. E. Deluca11, , J. McCaugheyJ. McCaughey11, K. K. Reeves, K. K. Reeves11, and M. Gros, and M. Gros33
1.1. Harvard-Smithsonian Center for Astrophysics, USA Harvard-Smithsonian Center for Astrophysics, USA 2. Purple Mountain Observatory, China2. Purple Mountain Observatory, China
3. DSM/DAPNIA/Service d’Astrophysique, CEA Saclay, France3. DSM/DAPNIA/Service d’Astrophysique, CEA Saclay, France
2007 SPD dissertation talk, Honolulu, 05/28/20072007 SPD dissertation talk, Honolulu, 05/28/2007
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AcknowledgementsAcknowledgements
• Advisors: Leon Golub (CfA), Guangli Huang (PMO)
• Collaborators: A. A. Van Ballegooijen, E. E. Deluca, J. McCaughey, K. K. Reeves, and M. Gros
• Valuable suggestions from S. K. Antiochos, J. Lin, J. Karpen, B. Schmieder…
• Other CfA SSXG group members: M. Weber, J. Cirtain, M. Bobra, P. J. Jibben, S. Saar, K. Korreck, A. Savcheva, L. Lundquist, and J. Bookbinder
• Instruments: TRACE, Hinode/XRT, SOHO/MDI, SOHO/LASCO, SOHO/EIT, NJIT/BBSO, SPI/ACS, Hinode/SOT, RHESSI
• Financial support: TRACE contract from Lockheed Martin and NASA contract NNM07AA02C at CfA
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OutlineOutline Background (Su et al. 2006, solar physics, 236, 325)
Statistical Analysis of Shear Motion (Su et al. 2007a, ApJ, 655, 606)
What Determines the Intensity of Solar Flare/CME events? (Su et al. 2007b, ApJ, 665, 1448)
Conclusions
Preliminary results from Hinode/XRT --Evolution of the sheared magnetic fields in AR10930 (Su et al. 2007c, PASJ, submitted)
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Shear Motion of Footpoints EUV brightening pairs
Start: close to the magnetic inversion line (MIL),
but widely separated along the MIL (Fig. a, highly sheared)
End: straight across and far from the MIL
(Fig. f, weakly sheared)
Strong-to-weak shear motion of the footpoints
Hard X-ray observations (Yohkoh/HXT) (Masuda, Kosugi, and Hudson 2001)
Hα, EUV, and microwave observations
(Su et al. 2006 and references therein)
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This observed shear change can be understood by the cartoon we made corresponding to the standard model for solar flares. (e.g., Moore et al. 2001 and references therein).
InterpretationInterpretation
Cartoon of the evolution of the magnetic field in the standard model of solar flares ( Su et al. 2006).
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OutlineOutline
Background (Su et al. 2006, solar physics, 236, 325)
Statistical Analysis of Shear Motion (Su et al. 2007a, ApJ, 655, 606)
What Determines the Intensity of Solar Flare/CME events?
(Su et al. 2007b, ApJ, 665, 1448)
Conclusions
Preliminary results from Hinode/XRT --Evolution of the sheared magnetic fields in AR10930 (Su et al. 2007c, PASJ, submitted)
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MotivationMotivation
Two Questions:
Is the shear motion of the footpoints common?Is the shear motion of the footpoints common?
Could the change from the impulsive to gradual phase be Could the change from the impulsive to gradual phase be related to the magnetic shear change?related to the magnetic shear change? (Lynch et al. 2004)(Lynch et al. 2004)
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Distribution of Shear AnglesDistribution of Shear Angles
Data sample: 50 two-ribbon flares well observed by TRACE
Type I flares: 86% (43 out of 50)
Ribbon separation: Yes Shear motion: Yes
For 24 Type I flares Initial shear angles: 50°– 80° Final shear angles: 15°– 55° Change of shear angles: 10°– 60°
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Distribution of Distribution of TEIP - TCSM
15 Type I flares
measured shear angle corresponding HXR observations
TEIP - TCSM: 0~2 min
In most events, the cessation of shear change is 0-2 minutes earlier than the end of the impulsive phase.
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OutlineOutline Background (Su et al. 2006, solar physics, 236, 325)
Statistical Analysis of Shear Motion (Su et al. 2007a, ApJ, 655, 606)
What Determines the Intensity of Solar Flare/CME events? (Su et al. 2007b, ApJ, 665, 1448)
Conclusions
Preliminary results from Hinode/XRT --Evolution of the sheared magnetic fields in AR10930 (Su et al. 2007c, PASJ, submitted)
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Data sets and methodsData sets and methods
Data sample: 18 Type I flares
associated with CMEs
measured shear angles
Six magnetic parameters:
Parameters representing magnetic size: Background field strength (B), the area (S), and magnetic flux ()
Parameters representing magnetic shear: Initial shear angle (), final shear angle (), and change of shear angle()
Intensity of flare/CME events:
Peak flare flux (PFF) and CME speed (VCME)
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Result IResult I
log10B, log10S, log10 vs. log10(PFF), VCME : positive correlations
log10 is better than log10B, log10S ( =B×S)
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Result IIResult II
vs. log10(PFF), VCME : no correlation
is better than both and ( = - )
, vs. log10(PFF), VCME : negative and positive correlations
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Result IIIResult III
Three multi-parameter combinations vs. log10(PFF) and VCME : strong linear correlations
Combination 2 (log10 , , ) is the top-ranked combination
Combination 2 is only slightly better than combination 3 (log10 , )
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OutlineOutline
Background (Su et al. 2006, solar physics, 236, 325)
Statistical Analysis of Shear Motion (Su et al. 2007a, ApJ, 655, 606)
What Determines the Intensity of Solar Flare/CME events? (Su et al. 2007b, ApJ, 665, 1448)
Conclusions
Preliminary results from Hinode/XRT --Evolution of the sheared magnetic fields in AR10930 (Su et al. 2007c, PASJ, submitted)
![Page 16: Magnetic Shear in Two-ribbon Solar Flares Yingna Su 1,2 Advisors: Leon Golub 1, Guangli Huang 2 Collaborators: A. A. Van Ballegooijen 1, E. E. Deluca 1,](https://reader036.fdocuments.in/reader036/viewer/2022062516/56649d565503460f94a3442f/html5/thumbnails/16.jpg)
ConclusionsConclusions
The strong-to-weak shear motion of the footpoints is a common feature in two-ribbon flares.
The cessation of magnetic shear change is 0-2 minutes earlier than the end of the impulsive phase in 10 out of the 15 events, which suggests that the change from impulsive phase to gradual phase is related to the magnetic shear change.
The magnetic flux and change of shear angle are two best parameters which show comparably strong correlations with the peak flare flux and CME speed. A multi-parameter combination showsbetter correlation than individual parameter.
The intensity of solar flare/CME events may depend mainly on the released magnetic free energy () rather than the total magnetic free energy () stored prior to the eruption.
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OutlineOutline Background (Su et al. 2006, solar physics, 236, 325)
Statistical Analysis of Shear Motion (Su et al. 2007a, ApJ, 655, 606)
What Determines the Intensity of Solar Flare/CME events? (Su et al. 2007b, ApJ, 665, 1448)
Conclusions
Preliminary results from Hinode/XRT --Evolution of the sheared magnetic fields in AR10930 (Su et al. 2007c, PASJ, submitted)
![Page 18: Magnetic Shear in Two-ribbon Solar Flares Yingna Su 1,2 Advisors: Leon Golub 1, Guangli Huang 2 Collaborators: A. A. Van Ballegooijen 1, E. E. Deluca 1,](https://reader036.fdocuments.in/reader036/viewer/2022062516/56649d565503460f94a3442f/html5/thumbnails/18.jpg)
Observational DataObservational Data Target:
NOAA AR 10930 where two X-class flares occurred:
X3.4 flare on 2006/Dec/13
X1.5 flare on 2006/Dec/14
Data from:
Hinode/XRT
Hinode/SOT
TRACE
SOHO/MDI
Topic:
Evolution of the sheared core field prior to, during, and after the flares.
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Formation of the sheared core fieldFormation of the sheared core field
XRT observations of sheared field formation:
From
00:19 UT on Dec 10
To
12:43 UT on Dec 12
SOT observations of
1. Emerging flux
2. West-to-east Motion
3. CCW Rotation
in the Lower sunspot
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
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Part of the sheared cored field erupted, while part of them stayed behind.
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
X 3.4 flare on 2006/12/13
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
X1.5 flare on 2006/12/14
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Pre-flare vs. post-flare sheared core field (Dec 13 flare)Pre-flare vs. post-flare sheared core field (Dec 13 flare)
Post-flare core field is less sheared than the pre-flare core field
Reformation or partial eruption of the filament
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Pre-flare vs. post-flare sheared core field (Dec 14 flare)Pre-flare vs. post-flare sheared core field (Dec 14 flare)
Post-flare core field is less sheared than the pre-flare core field
Reformation or partial eruption of the filament
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SummarySummary
The formation of the sheared core field is caused by the CCW rotation and west-to-east motion of an emerging sunspot.
XRT observations of partial eruption of the sheared core field may explain the existence of the filament after the flare.
Post-flare core field is much less sheared than the pre-flare core field, which is consistent with the scenario that the energy released during the flare is stored in the highly sheared core field.
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Thank you Thank you for for
your attention !your attention !
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Part of the sheared cored fields erupted, Part of the sheared core fields stayed behind