Jet Phenomena in the Solar Atmosphere with RotationalEruption or Spinning Motion;

Observation associated with Our MHD numerical Simulations

2004年 4月 12日宮腰　剛広

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 fieldsThe mass in the high density twisted loop is driven put into the open flux tubedue 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 magnetictwist) is formed.

NOAA 4474, 23 April 1984

Ha -5.0A

Ha +-0A

A, B: delta type sunspots

p: preceding f: following

activity:A>>B

22:35 / 23, Apr

22:05 / 24, Apr

Ap: westward motionBf : 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 lineweak shear

A: filament parallel to neutral linestrong shear

Two X class flares on A:04 UT on 24 Apr00 UT on 25 Apr

B: no strong flare

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

... but erupting process is clearly seenin Ha wing

The curling fine structures of thefilament indicate unwinding rotational motion of the spoutingmaterial along the axis of the filament.

velocitygrams

Ha +-1.0 or +- 0.8

white: the velocity toward the observerblack: the velocity away from us

with the photographic subtraction method(Leighton et al. 1962)

EF : erupting filamentPFL : downward motions in the post-flare loops

EF: left part, black right part, whiteclear separation indicates the rotatingmotion around the spouting axis of thefilament

The direction of the rotation coincideswith that of the detwisting of the helicaltwist found in Figure 4.

EF

SE : secondary eruption

my left the chromosphere around00:43 UT

microwave absorption was observed00:50 – 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 thesunspots and post-flare loops

the velocity of the erupting filamentprojected to the sky plane:120 km/s

rotational : 50km/s (Figure 6)

50 km/s (rotation) must be larger thanthe line-of-sight component of the ascendingvelocity. Otherwise, the clear separation of black and white along the filament axiscannot be seen so clearly in the velocitygrams

line of sight

rising

from side

shita

120:projection to the sky

5050

120

shita

120/tan(shita)<50,shita>68

rising filament almost normalto the line-of-sight

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 eruptingfilament cloud.

21:38, 25/Apr22:07, 24/Aprtwo hours before the flare

neutralline

F: nearly parallelT: large angle

filament // neutralstrong shear

filament normal neutralweak shear

twistedObserved characteristicsagree well with those derivedfrom the simulation of Shibataand Uchida (1986)

Yohkoh and Mees NOAA 7260, 1992 Aug 19-20 The 23:11 UT Event

Yohkoh SXTContour: SXT, image: Mees, Ha

footpoint:saturated

P0a

Expanded image of the footpoint

only this time is saturated

it consists of two loops

upper and lower parts oftenhave different brightness

F: footpointsL: interfootpoint regions

The light curves of these regions aresignificantly different.These images and light curves showthat the flaring X-ray structure consistsof two loops that are contiguous, endto end.

bright point (Ha)

SXT loop

surge

grayscale: IVM magnetogram

SXT contour

polarityinversionline

-, near the moving satellite spots

+, near satellite

-, weaker fieldno spot

SXT

Ha blue Ha red

Ha center

23:11:30

Ha velocity contours reveal thelocation of the 23:11surge due to itsrotational motion

angular rate:10^-3 rad/s,lasting 1000 s

the spin is right handed(all the surges in table 1)

six of nine surge/jetevents show highly localized Ha downflow at a bright point at the base of the surge, andeight of nine events showthat the surge is locatedover 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

fig6 area

SXT

Ha center

(maximum value)

stage 1: blueshifts graduallydevelop. Ha gradually brightensalthough no-Xray brighteningsupports that this is Dopplerbrightening.

stage 2: Ha brightens dramaticallyand X-ray emission begins to increase.

stage 3: X-rays peak and a strong redshift appears and peaks witha delay of about 1 minute with respectto the time of peak blueshift.

(surge base downflow motion)

The 18:34 UT event

in contrast to the previous event, it appears to occur in a plane that is considerablyinclined to the line of sight.

figure 9 area

Ha

X-ray

X-ray Jet

Ha surge

not cospatial

(fig8 box)

Ha line center

black: blue shiftwhite: red shift

period A: two small penumbral filamentsone is more curved than the otherThe end of the one rears up in a whiplike manner, while the other remains in place.

Period B: two brighteningsapproach one another (20 km/s)This converging footpoints phenomenonhas not reported before.

period C: A blueshifted (dark) linear structureappears in all images, moving from right toleft 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 averages25 km/s, peaks 120 km/s

The bipole associatedwith the moving satellitespots and Ha penubbralfilaments

cool plasma moves,caused Dopplerbeightenings in Haweak reconnection,(bit strongly heated)

strong heating beginsHa surges above X-rayjet

downward

reconnectionbetween open fieldsand stronglytwisted bipoleloops(Shibata & Uchida 1986)

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

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

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 )