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Solar seminor: 4 Oct. 2004

Solar seminor: 4 Oct. 2004. Eruption of a multiple-turn helical magnetic flux tube in a large flare : Evidence for external and i ternal reconnection that fits the breakout model of solar magnetic eruptions G.Allen Gary and R.L. Moore

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Solar seminor: 4 Oct. 2004

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  1. Solar seminor: 4 Oct. 2004 • Eruption of a multiple-turn helical magnetic flux tube in a • large flare : Evidence for external and iternal reconnectionthat fits the breakout model of solar magnetic eruptions • G.Allen Gary and R.L. Moore • Astrophys. J. 611 545-556 (2004 August 10) (2) Optical Design for a New Off-axis 1.7m Solar telescope (NST) at Big Bear Leonid Didkovsky, Jeff Kuhn and Phil Goode BBSO preprint # 1188 Submitted to the SPIE Proc.5171 (San Diego,3-8 August 22003)

  2. (1)Eruption of a multiple-turn helical magnetic flux tube in a large flare : Evidence for external and iternal reconnection that fits the breakout model of solar magnetic eruptions G.Allen Gary and R.L. Moore Astrophys. J. 611 545-556 (2004 August 10) In this talk: Firstly: Introduce the main observational results and the flare model of this paper. Secondly: Point out the mistakes in this model. Thirdly: Propose more detailed analyses of the evoluving magnetic field configulation and flare developing senario of this interesting region to get more realistic flare senario.

  3. (1) Introduction Analysis of the complex event of the X3 flare of 2002July15, 20:04UT Liu et al.(2003 Ap. J. Letter 593, L137): discussed the development of erupting multiple-turn flux rope in 160nm images in the scope of the standard flare model.

  4. Fig.1 Multiple-turn helix in the X3 flare of 2002July15

  5. The main observational point noticed in this paper: The initiation of the helix eruption starts about 25s after the impusive microwave burst peak.

  6. The important finding of this paper: The observations are counter to the standard flare model and support the breakout model for the flare onset.

  7. 2. Observations Fig.2 MSFC vector magnetogram MDI Mgnetogram at 10:56 UT

  8. Fig.3 SOON Learmonth/SEC Hα image at 05:42UT

  9. Fig.4. TRACE 160nm images

  10. Fig.5 Time profiles of GOES X-ray and OVSA μwave flux

  11. 1st CME 20:30 UT 21:06 UT 20:05 UT 2nd CME 21:30 UT 22:06 UT 02:18 UT Fig.6 LASCO CME (C2: 2-6R, C3:3.7-32R)

  12. 3. Analysis Fig. 7 Side view and top view of the potential field computed from MDI Note: Lb and Lc are not potetial but strongly sheared.

  13. Fig.8 Left:Enlargement of TRACE omage. Right: Set of field lines defining the separatrix

  14. Fig.9:Topological sketches of the main components of the eruptions t~20:05 UT t~19:50 UT • Mistakes: • E4 is not on F3. • No description of the • importrant fact that the • first two ribbon flare or • the primary energy • release occurred • over the Lc • (3) No explanation of the • primary energy release • or the μwave burst peak • between the stages ① • and ②. • (4) At the stage ②, R1ribbon • has already formed. t~20:15 UT t~20:10 UT t~20:41 UT

  15. Fig 10 velocity profiles of the erupting helix

  16. 4. Summary and Discussion Observations show • The initial impulsive phase occurred • before the first core eruption • (2) The initial brightnenings are distant • from the neutral lines and agree with • reconnection at the null The observations support the breakout model over the Standard model for the initiation of the X3 flare. However, the upper reconnection site of the breakout has yet to be directly observed.

  17. TRACE 160nm movie Made by S. Saito

  18. MDI magnetogram movie of 10030 region Made by S. Saito

  19. Essential points to be studied for more realistic model: (1) How was the complex magnetic field configuration formed? (2) What triggered the first energy release over the sheared neutral line Lc? (3) The role of the emerging twisted flux loops at the NW part of the spot P3 noted by Liu et al. (4) The expanding flare ribbon and flare loops collided to the neighboring sheared filament field and triggered the second and the third flares. P3 Lc

  20. (2) Optical Design for a New Off-axis 1.7m Solar telescope (NST) at Big Bear Leonid Didkovsky, Jeff Kuhn and Phil Goode BBSO preprint # 1188 Submitted to the SPIE Proc.5171 (San Diego,3-8 August 22003)

  21. Introduction First light for NST: 2005 Full Operation: 2006 NST will achieve 0.08 arcsec or 56 km on the solar surface. NST will cover the wavelength range from 390 nm to far-infrared.

  22. 2. NST requirements

  23. 3. Telescope opticcal design

  24. A result of preliminary finite element analysis model with 36 actuators for the NST primary mirror

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