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Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 . 2005,ApJ, 622 ,1251. J. Lin , Y.-K. Ko, L. Sui, J. C. Raymond, G. A. Stenborg, Y. Jiang, S. Zhao, and S. Mancuso. 2005/11/28 太陽雑誌会 <short> 長島薫 Solar Seminar (Zasshikai) NAGASHIMA Kaori.
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Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 2005,ApJ, 622,1251 J. Lin, Y.-K. Ko, L. Sui, J. C. Raymond, G. A. Stenborg, Y. Jiang, S. Zhao, and S. Mancuso 2005/11/28 太陽雑誌会 <short> 長島薫 Solar Seminar (Zasshikai) NAGASHIMA Kaori
<1.Introduction> Since the timescale of magnetic dissipation or reconnection is longer than that of the catastrophe (i.e., the Alfven timescale ), the development of a long current sheet is expected during major eruptions. In this study, a direct observation of the current sheet and the associated reconnection process is reported. reconnection inflow current sheet & reconnection outflow part of Fig.1 Schematic diagram of a disrupted magnetic field forming in an eruptive process.
<2.Observations & Results>Observations an eruptive event • occurred on 2003 Nov. 18 • on the east limb (between NOAA AR 0507 & 0508) DATA: • SOHO/EIT 195Å & RHESSI • observation of the initial stage & subsequent development of the eruption in the lower corona • SOHO/UVCS, LASCO & MLSO MK4 • observation of the consequences in the higher corona
EIT 195Åmovies current sheet (fig2) flare loop (fig2)non-movie
composite of LASCO C2 (17:50) , MK4(17:49) ,& EIT 195Å (17:48) images This figure resembles the typical Kopp-Pneuman configuration for major flares (Kopp & Pneuman 1976), in which the post-flare/CME loops are located under the cusp structure at the lower tip of the current sheet. Fig. 8
after the wavelet-based intensity contrast enhancement (WICE) before the WICE WICE → good at emphasizing the fine features of large-scale structure.(Stenborg & Cobelli 2003 A&A)
LASCO C2 movie • enhanced by the wavelet (WICE) technique • Fine structures • leading edge & core of CME • current sheet • the helical structure around the CME core fig4 (~12hr)
<2. Observations & Results>Inflow Velocity & Reconnection rate • Following Yokoyama et al.(2001), the inflow velocity can be measured using the motion of two legs of the arcade system observed by EIT. • However, the structure seen in the EIT images is diffuse and the apparent inward motion was suggested that actually due to the changing position of the X-type reconnection region rather than inflow. (Chen et al. 2004) • Therefore, in this study, they use the UVCS observations to determine the inflow speed. Yokoyama et al. 2001 part of Fig.4
Fig.5 EIT 195Å (10:14) UVCS Lyα(slit scan) LASCO C2 (10:26) using WICE The width of a dark gap seen in the left UVCS image decreased with time. magnetic reconnection inflow time *dark gap ⇔ current sheet
<2. Observations & Results>Inflow Velocity & Reconnection rate • The dark gap (not a no emission region but a lower Lyα intensity region) could result from a higher temperature or a significant outflow speed. • The Lyα width in the gap is considerably larger than in the outside of it. This suggests higher temperature in the gap. However, this temperature (6.7e6 K) require a density above 1e8 /cm^3 to account for the Lyα intensity. This is inconsistent with no FeXVIII signal. • Smaller density also can be a cause of darkening, but the modest density enhancement was observed in the LASCO images. • Then, the low emission is due to Doppler dimming. • An outflow speed of 200 km/s would account for the low intensity in the gap. (large line width⇔LOS comp. of outflow.)
<2. Observations & Results>Inflow Velocity & Reconnection rate Inflow velocity can be deduced by comparing the widths of the gap every two successive times. inflow velocity VR : 10.5-106 km/s north time the center of gap ~ P.A. =95° south Lyα intensity Position Angle [deg.] Fig.11a 5 Lyαintensity profiles along the UVCS slit taken at 1.70Rsun 10:04-10:14 UT.
an evidence for the reconnection inflow LOS ⊥inflow north : blueshift (~20km/s) No Doppler shift south : redshift (~35km/s) inflow inflow When the field lines adjoining the CS are tilted ... the center of the gap Wavelength [A] Fig. 12 averaged over 10:04-10:14
<2. Observations & Results>Inflow Velocity & Reconnection rate • Outflow velocity : 460-1075 km/s • Several bright blobs successively flowed away from the Sun along a long thin streamer-like feature observed by LASCO C2 & C3. • the thin feature ⇔current sheet (CS) • the blobs ⇔ outflow of reconnection inside the CS • Assuming an incompressible plasma, the outflow velocity is equal toVA(the local Alfven speed in the reconnection region). • Therefore, the reconnection rate MA=VR/VA is in the range from 0.01 to 0.23. (However the real value of MA should vary over a wider range.)
Summary • an erupitive process • direct observation of CS, inflow, and outflow • an energetic CME • the CME & the flare are connected by a stretched current sheet. • the average reconnection inflow :10.5-106km/s (using the UVCS Lyα data ) • Lyα profiles around the gap are shifted. • a direct evidence of the reconnection inflow? • the average outflow : 460-1075km/s (blob) • the reconnection rate :0.01-0.23