1. Jet Phenomena in the Solar Atmosphere with Rotational Eruption or Spinning Motion; Observation associated with Our MHD numerical Simulations 2004 年 4 月 12 日 宮腰 剛広

4. Jets associated with Rotating Eruption or Spinning Motion Kurokawa et al. 1987, Solar Phys., 108, 251 Canfield et al. 1996, Apj, 464, 1016 Pike and MASON, 1998, Solar Phys., 182, 333 Alexander and Fletcher, 1999, Solar Phys., 190, 167 Observations Theory Shibata and Uchida, 1986, Solar Phys. magnetic twist packet propagates open coronal fields The mass in the high density twisted loop is driven put into the open flux tube due to both pinch effect and JXB force at the front of the packet. Hot core (by pinch effect) and Cool sheath (unwinding front of the magnetic twist) is formed.

5. NOAA 4474, 23 April 1984 Ha -5.0A Ha +-0A A, B: delta type sunspots p: preceding f: following activity: A>>B

6. 22:35 / 23, Apr 22:05 / 24, Apr Ap: westward motion Bf : eastward motion (motion with emergence) C, Af: not clear motion AFS : Ap and Bf (opposite polarities) neutral line filament (fig2,a) B: filament normal to neutral line weak shear A: filament parallel to neutral line strong shear Two X class flares on A: 04 UT on 24 Apr 00 UT on 25 Apr B: no strong flare

7. X13: 00 UT on 25 Apr Ha center (a)pre flare (b) great two ribbon flare occurred (b)(c) helically twisted structure (c)(d) helical twists are gradually untwisted (e) started to spout up of untwisting rotation (f) filament is hardly visible in Ha line center

8. ... but erupting process is clearly seen in Ha wing The curling fine structures of the filament indicate unwinding rotational motion of the spouting material along the axis of the filament.

9. velocitygrams Ha +-1.0 or +- 0.8 white: the velocity toward the observer black: the velocity away from us with the photographic subtraction method (Leighton et al. 1962) EF : erupting filament PFL : downward motions in the post-flare loops EF: left part, black right part, white clear separation indicates the rotating motion around the spouting axis of the filament The direction of the rotation coincides with that of the detwisting of the helical twist found in Figure 4.

11. EF SE : secondary eruption my left the chromosphere around 00:43 UT microwave absorption was observed 00:50 – 00:58 at TRO (Enome 1985); good temporal coincidence the second ejection extended along the line S in Figure 7 and absorbed the microwave radiation emitted by the sunspots and post-flare loops

12. the velocity of the erupting filament projected to the sky plane: 120 km/s rotational : 50km/s (Figure 6) 50 km/s (rotation) must be larger than the line-of-sight component of the ascending velocity. Otherwise, the clear separation of black and white along the filament axis cannot be seen so clearly in the velocitygrams line of sight rising from side shita 120: projection to the sky 50 120 shita 120/tan(shita)<50, shita>68 rising filament almost normal to the line-of-sight

13. R : NRO (Figure 7) moving type IV bursts, 200-830 km/s (Figure 8) angle between R and P is small (<15 deg), so directly compared in Figure 8 It is obvious that the moving type IV burst is closely connected to the erupting filament cloud.

14. 21:38, 25/Apr 22:07, 24/Apr two hours before the flare neutral line F: nearly parallel T: large angle filament // neutral strong shear filament normal neutral weak shear twisted Observed characteristics agree well with those derived from the simulation of Shibata and Uchida (1986)

15. Yohkoh and Mees NOAA 7260, 1992 Aug 19-20The 23:11 UT Event Yohkoh SXTContour: SXT, image: Mees, Ha footpoint: saturated P0a

16. Expanded image of the footpoint only this time is saturated it consists of two loops upper and lower parts often have different brightness

17. F: footpoints L: interfootpoint regions The light curves of these regions are significantly different. These images and light curves show that the flaring X-ray structure consists of two loops that are contiguous, end to end.

18. bright point (Ha) SXT loop surge

19. grayscale: IVM magnetogram SXT contour polarity inversion line -, near the moving satellite spots +, near satellite -, weaker field no spot

20. SXT Ha blue Ha red Ha center 23:11:30 Ha velocity contours reveal the location of the 23:11 surge due to its rotational motion angular rate: 10^-3 rad/s, lasting 1000 s the spin is right handed (all the surges in table 1)

21. six of nine surge/jet events show highly localized Ha downflow at a bright point at the base of the surge, and eight of nine events show that the surge is located over the outer loop downflow region is located at the base of the surge It is at the north footpoint of the north loop, i.e., the footpoint farthest from p0a

22. fig6 area SXT Ha center (maximum value) stage 1: blueshifts gradually develop. Ha gradually brightens although no-Xray brightening supports that this is Doppler brightening. stage 2: Ha brightens dramatically and X-ray emission begins to increase. stage 3: X-rays peak and a strong redshift appears and peaks with a delay of about 1 minute with respect to the time of peak blueshift. (surge base downflow motion)

23. The 18:34 UT event in contrast to the previous event, it appears to occur in a plane that is considerably inclined to the line of sight. figure 9 area Ha X-ray X-ray Jet Ha surge not cospatial

24. (fig8 box) Ha line center black: blue shift white: red shift period A: two small penumbral filaments one is more curved than the other The end of the one rears up in a whiplike manner, while the other remains in place. Period B: two brightenings approach one another (20 km/s) This converging footpoints phenomenon has not reported before. period C: A blueshifted (dark) linear structure appears in all images, moving from right to left along a path parallel to the penumbral filament that showed whiplike motion in strip A.The measured transverse speed of propagation of the blueshift region averages 25 km/s, peaks 120 km/s

25. The bipole associated with the moving satellite spots and Ha penubbral filaments cool plasma moves, caused Doppler beightenings in Ha weak reconnection, (bit strongly heated) strong heating begins Ha surges above X-ray jet downward reconnection between open fields and strongly twisted bipole loops (Shibata & Uchida 1986)

26. The observed a: 0.4/Mm (Leka et al. 1994) length of filaments: l~20Mm, stored twist is several radians. 10^-3 radian times 10^3 s equal 1 radian. strong of twist is enough moving blueshift with whiplike motions conversing footpoints

27. Alexander and Fletcher, 1999, Solar Phys., 190, 167 TRACE observation

28. Vy component + - emerging flux region x z y Vy x z Vy （紙面垂直速度成分） 赤：＋ 青：－ ( コロナアルフベン速度の 約 10% ぐらい )