1. 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

2. 1) Solar Source Region: AR 8210 2) MDI Full-Disk, Carrington Rotation 1935 **

3. 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!

4. 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

5. 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 **

6. 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 **

7. Helio- & Magnetospheric in situ Data Multiple-CMEs  Disturbed IP environment! –Effects of CME #1 difficult to discern ACE/WIND Data: Shock, Southward B z * * CME #2 was significantly geoeffective **

8. 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.

9. Basis for Selection as SHINE Event CME #2 is well-observed on disk in multiple data sets, and was strongly geoeffective.

10. Poster Previews Loraine Lundquist et al.* (#48)* Manolis Georgoulis & B. La Bonte * (#51)* Dana Longcope * (#7)* Ilia Roussev et al. * (talk tomorrow, WG #2)*

11. 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!

12. 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! 

13. MDI Full-Disk, Carr. Rot.1935 (BACK)

14. MDI Sub-region, 11:00 UT 1 May – 00:20 UT 3 May (BACK)

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

16. 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. (BACK)

17. GOES Flare Data, 1-3 May 1998 CME #1 CME #2 (*)

18. Coronal Topology, from Sterling & Moore (2001) (*)

19. Yohkoh SFD Images, 1-2 May (BACK) FAST

20. Yohkoh SFD Images, 1-2 May (BACK) SLOW

21. EIT 195 Movie (*)

22. LASCO C2 Difference Movie, 1May (BACK)

23. LASCO C2 Difference Movie, 2May (BACK)

24. Kanzelhöhe Sol. Obs. H  Flare Images (BACK)

25. Moreton Wave, Pohjolainen et al. (2002) (BACK)

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

27. Radio Timings, Pohjolainen et al. (2002) (BACK)

28. Radio Sources, Pohjolainen et al. (2002) (*)

29. Timeline, Pohjolainen et al. (2002)

30. Dimmings, Pohjolainen et al. (2002) (BACK)

31. Solar Wind Data, ACE (BACK)

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