SHINE Campaign Event: 12 May 1998 Brian Welsch

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SHINE Campaign Event 1-2 May 1998Brian Welsch
( Yan Li)Space Sciences Laboratory, UC Berkeley

• Introduction Data, Context, etc.
• Work Completed Ongoing
• Poster Previews!
• The Punchline
• Primarily Interested in Two Halo CMEs
• 2230 UT 1 May 1330 UT 2 May

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1) Solar Source Region AR 8210

• 2) MDI Full-Disk, Carrington Rotation 1935

3
Photospheric Field Evolution

• Sub-Region of MDI Full-Disk Movies
• 1100 UT 1 May -- 0020 UT 3 May (37 hr)
• LCT velocities from subset of these data
• Notable evolution
• 1) Rotational motion injects energy, helicity
• 2) Flux cancellation creates flux rope?
• AR flows are hot topic three new methods to find
  3-D flows, e.g., ILCT
• More about flows in Poster previews!
• Modelers using these data to simulate eruptions!

4
Development in Low Corona

• Yohkoh SXT Connections with AR 8214!
• CMEs global? Model-in-box problematic?
• Nearby coronal hole?
• CME-associated GOES Flares
• M-class _at_ 2230 UT 1 May,
• X-Class _at_ 1332 UT 2 May

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Development of CME 1

• Pre H-a /EIT crinkles away from core
  indicative of breakout-type reconnection?
  (Sterling Moore, 2001)
• EIT 195 Movie, S. Regnier
• Halo CME, LASCO C2

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Development of CME 2

• Ha Images (Kanzelhöhe Sol. Obs.)
• Blast Waves Pohjolainen et al., 2002
• Wills-Davey Warmuth et al., 2001
• Radio Sources Pohjolainen et al., 2002
• Post Dimmings in SXT
• Halo CME

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Helio- Magnetospheric in situ Data

• Multiple-CMEs ? Disturbed IP environment!
• Effects of CME 1 difficult to discern
• ACE/WIND Data Shock, Southward Bz
• CME 2 was significantly geoeffective

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Basis for Selection as SHINE Event

• CME 1 also chosen as a MURI Event, for driving
  coronal MHD codes from magnetograms (see Bill
  Abbetts talk, tomorrow a.m., WG I.)
• time series of Imaging Vector Magnetograph (IVM)
  data prior to flare eruption
• Good data coverage! But interpretation of CME
  1s effects in situ CME 1 arent clear.

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Basis for Selection as SHINE Event

• CME 2 is well-observed on disk in multiple data
  sets, and was strongly geoeffective.

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Poster Previews

• Loraine Lundquist et al. (48)
• Manolis Georgoulis B. La Bonte (51)
• Dana Longcope (7)
• Ilia Roussev et al. (talk tomorrow, WG 2)

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Take Home Points, a.k.a. The Punchline

• Used Data to Display Event Context
• Introduced Completed and Ongoing Work
• Including some presented at this meeting!
• GOAL Generate Consensus Report!
• Special issue of JGR?
• Living article?
• Much work to be done!

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And so, my fellow physicists

• Ask not what SHINE can do for you,
• but what you can do for SHINE!
• We need your data!
• We need your effort!

? Special Thanks to Yan Li! ?
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MDI Full-Disk, Carr. Rot.1935
(BACK)
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MDI Sub-region, 1100 UT 1 May 0020 UT 3 May
(BACK)
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Fourier LCT (FLCT) Velocities,1100 UT, 1 May
0020 UT, 3 May
(BACK)
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ILCT flows, c. 1940 UT, 1 May

• Inductive LCT, combined with vector magnetic
  field data, enables us to find 3-D flow field
  transverse flows are shown as arrows, up/down
  flows shown as blue/red contours.

(BACK)

• For more details, see George Fishers poster 96

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GOES Flare Data, 1-3 May 1998
CME 2
CME 1
()
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Coronal Topology, from Sterling Moore (2001)
()
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Yohkoh SFD Images, 1-2 May
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FAST
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Yohkoh SFD Images, 1-2 May
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SLOW
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EIT 195 Movie
()
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LASCO C2 Difference Movie, 1May
(BACK)
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LASCO C2 Difference Movie, 2May
(BACK)
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Kanzelhöhe Sol. Obs. H? Flare Images
(BACK)
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Moreton Wave, Pohjolainen et al. (2002)
(BACK)
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TRACE wave diff. movie (M.Wills-Davey)1
(BACK)
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Radio Timings, Pohjolainen et al. (2002)
(BACK)
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Radio Sources, Pohjolainen et al. (2002)
()
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Timeline, Pohjolainen et al. (2002)
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Dimmings, Pohjolainen et al. (2002)
(BACK)
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Solar Wind Data, ACE
(BACK)
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Petrinec et al. (1998) Movie of Bow Shock,
Magnetopause
(BACK)