solar seminor: 4 oct. 2004

Solar seminor: 4 Oct. 2004

(1)Eruption of a multiple-turn helical magnetic flux tube in a large flare : Evidence for external and iternal reconnection th

at 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)

(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.

(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.

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

The main observational point noticed in this paper:

The initiation of the helix eruption starts about 25s after the impusive microwave burst peak.

The important finding of this paper: The observationsare counter to the standard flare model and supportthe breakout modelfor the flare onset.

2. Observations

Fig.2

MSFC vectormagnetogram

MDIMgnetogramat 10:56 UT

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

Fig.4. TRACE 160nm images

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

Fig.6 LASCO CME (C2: 2-6R, C3:3.7-32R)

20:05 UT 20:30 UT 21:06 UT

21:30 UT 22:06 UT 02:18 UT

1stCME

2nd CME

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.

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

Fig.9:Topological sketches of the main components of the eruptionsMistakes:

(1) E4 is not on F3.(2) 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 , R② 1ribbon

has already formed.

t~19:50 UTt~20:05 UT

t~20:10 UTt~20:15 UT

t~20:41 UT

Fig 10 velocity profiles of the erupting helix

4. Summary and Discussion

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.

(1)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

Observations show

TRACE 160nm movie

Made by S. Saito

MDI magnetogram movie of 10030 region

Made by S. Saito

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.

Lc

P3

(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)

1. Introduction

First light for NST: 2005Full 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.

2. NST requirements

3. Telescope opticcal design

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