SHINE Campaign Event: 1-2 May 1998 Brian Welsch (& Yan Li) Space Sciences Laboratory, UC Berkeley Introduction: Data, Context, etc. Work: Completed & Ongoing.

SHINE Campaign Event: 1-2 May 1998

Brian 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:

22:30 UT 1 May & 13:30 UT 2 May

1) Solar Source Region: AR 8210

2) MDI Full-Disk, Carrington Rotation 1935

Photospheric Field Evolution• Sub-Region of MDI Full-Disk Movies

– 11:00 UT 1 May -- 00:20 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!

Development in Low Corona

• Yohkoh SXT: Connections with AR 8214! – CMEs global? Model-in-box problematic?– Nearby coronal hole?

• CME-associated GOES Flares: 1. M-class @ 22:30 UT 1 May,

2. X-Class @ 13:32 UT 2 May

Development of CME #1

• Pre: H- /EIT crinkles away from “core” indicative of breakout-type reconnection? (Sterling & Moore, 2001)

• EIT 195 Movie, S. Regnier

• Halo CME, LASCO C2

Development of CME #2

• H 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 *

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 *

Basis for Selection as SHINE Event

• CME #1 also chosen as a MURI Event, for driving coronal MHD codes from magnetograms (see Bill Abbett’s 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 #1’s effects in situ CME #1 aren’t clear.

Basis for Selection as SHINE Event

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

Poster Previews

• Loraine Lundquist et al.* (#48)

• Manolis Georgoulis & B. La Bonte * (#51)

• Dana Longcope * (#7)

• Ilia Roussev et al. * (talk tomorrow, WG #2)

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

• Used Data to Display Event Context

• Introduced Completed and Ongoing WorkIncluding some presented at this meeting!

• GOAL: Generate ‘Consensus Report!’– Special issue of JGR? – ‘Living’ article?

• Much work to be done!

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!

MDI Full-Disk, Carr. Rot.1935

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MDI Sub-region, 11:00 UT 1 May – 00:20 UT 3 May

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Fourier LCT (FLCT) Velocities,11:00 UT, 1 May – 00:20 UT, 3 May

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ILCT flows, c. 19:40 UT, 1 May

For more details, see George Fisher’s poster #96

• 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.

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GOES Flare Data, 1-3 May 1998

CME #1

CME #2

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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

Yohkoh SFD Images, 1-2 May

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SLOW

EIT 195 Movie

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LASCO C2 Difference Movie, 1May

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LASCO C2 Difference Movie, 2May

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Kanzelhöhe Sol. Obs. H Flare Images

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Moreton Wave, Pohjolainen et al. (2002)

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TRACE wave diff. movie (M.Wills-Davey)1

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Radio Timings, Pohjolainen et al. (2002)

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Radio Sources, Pohjolainen et al. (2002)

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Timeline, Pohjolainen et al. (2002)

Dimmings, Pohjolainen et al. (2002)

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Solar Wind Data, ACE

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Petrinec et al. (1998) Movie of Bow Shock, Magnetopause

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