may98_plenary

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					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-a /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
• 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 *
   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 Work
  Including 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




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




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




                               (BACK)
ILCT flows, c. 19:40 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 Fisher’s poster #96
GOES Flare Data, 1-3 May 1998
               CME #2

          CME #1




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




                                             (*)
Yohkoh SFD Images, 1-2 May




                        (BACK)

                         FAST
Yohkoh SFD Images, 1-2 May




                        (BACK)

                         SLOW
EIT 195 Movie




                (*)
LASCO C2 Difference Movie, 1May




                                  (BACK)
LASCO C2 Difference Movie, 2May




                              (BACK)
Kanzelhöhe Sol. Obs. Ha Flare Images




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




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




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




                                (BACK)
Radio Sources, Pohjolainen et al. (2002)




                                           (*)
Timeline, Pohjolainen et al. (2002)
Dimmings, Pohjolainen et al. (2002)




                               (BACK)
Solar Wind Data, ACE




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




                                              (BACK)

				
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