Yan Li, Benjamin Lynch, Janet Luhmann SSL UC Berkeley€¦ · The Magnetic Cloud of Dec. 14-15,...
Transcript of Yan Li, Benjamin Lynch, Janet Luhmann SSL UC Berkeley€¦ · The Magnetic Cloud of Dec. 14-15,...
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Source region magnetic field of STEREO CMEs
Yan Li, Benjamin Lynch, Janet LuhmannSSL UC Berkeley
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The Magnetic Cloud of Dec. 14-15, 2006 at ACE and STEREO IMPACT A Li, Lynch and Luhmann
SSL UC Berkeley
MC
• ACE at L1 Observed the ICME at ~900km/s.
• Left: T, Np, Vx, Dyn, Br,t,n, |B|.
• The ICME shock arrived at ~1400UT, and MC ~2300UT.• STEREO IMPACT(A) IMF (Red) are overplotted on ACE data (Black). The ICME has a ~25min delayed at IMPACT, but features are otherwise almost identical.
~900km/s
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SOHO LASCO Halo CME on 2006/12/13 02:54:04 UT
Li, Lynch and LuhmannSSL UC Berkeley
1774 km/s (CME catalog, Yashiro et al.)
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Dec-13-2006 flare and CME
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1774 km/s
Yashiro et al.
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The Active region (AR10930) observed in multi-wavelength
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PhotosphereMagnetic Field
AR10930
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Chromosphere Magnetic Field
AR10930
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AR magnetc field andEvolution (MDI 96min)Dec 09 to 13, 2006
EruptionTime
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Dec 13 2006 flare (HINODE SOT)
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Left: Global solar magnetic field (MDI) for Dec. 13, 2006.The large active region (AR)10930 is the source regionof the CME.
PFSS model based on MDI synoptic map.Above: coronal holes and streamer arcade.Right: 3D streamer arcade on magnetogram
with center view of AR10930.(Blue: + Red: - )
Li, Lynch and LuhmannSSL UC Berkeley
AR10930
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Above: 3D streamer arcade and AR10930. Top-right: Field arcades from photosphere to source surface over the erupting neutral line. No magnetic null point found at this resolution, but finer scale will be analyzed.Bottom-right: Near surface field arcades over the erupting neutral line.
Li, Lynch and LuhmannSSL UC Berkeley
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The Magnetic Cloud of Dec. 14-15, 2006 at ACE and STEREO IMPACT A
• STEREO IMPACT(A) IMF (Red) are overplotted on ACE data (Black).
•The dashed lines mark the leading and trailing boundaries of the Magnetic Cloud.
•The MC fluxrope orientation (see Ying Liu et al.) agrees better with the overlying streamer belt, and nearly orthogonal with the erupting neutral line and post-flare arcade.
Li, Lynch and LuhmannSSL UC Berkeley
MC
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CME May-19-2007 13:24UT 958km/s (LASCO CME catalog, Yashiro et al.)
C2 difference images C3 difference images
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The eruption on May-19-2007 wavelet enhanced STEREO EUVI
anaglyph movies by Dr. Guillermo Stenborg
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Yashiro et al.
958km/s
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The Active region (AR10956) observed in multi-wavelength
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PhotosphereMagnetic Field
AR10956
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Chromosphere Magnetic Field
AR10956
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Erupting Filament19-May-2007(BBSO Hαnetwork)
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After the Eruption20-May-2007(BBSO Hαnetwork)
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AR10956 inSoft X-Ray(HINODE)before the eruption
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AR10956 inSoft X-Ray(HINODE)after theeruption
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Trace and others?AR10956 In EUV171(TRACE Mosaic)May 19 00:09 UT
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Trace and others?AR10956 In EUV171(TRACE Mosaic)May 21 00:09 UT
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AR magnetc field andEvolution (MDI 96min)May 17 to 21, 2007
Eruption Time
May 17 May 21
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Vector magetic field (NSO SOLIS)on May 15 and 22
1000 G 600 G
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MDI synoptic mapA proxy of the globalsolar magnetic field.White: + Black: -
Coronal magneticStructure by PFSS modelRed: coronal holes -;Orange and aqua lines: streamer belt;Purple: heliospheric current sheet;Green lines: equatorial field lines.Blue: coronal holes +
AR 10956
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Summary plots and events page athttp://sprg.ssl.berkeley.edu/impact/
• http://sprg.ssl.berkeley.edu/impact/data_browser.html
STEREO-A IMPACT STEREO-B IMPACTMay 21 – May 23, 2007
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Goals
• CME initiation• CME and ICME connection