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(2) 2. 26-AUG-92 20:44:52-22:58:50 1400. 1000. 1300. 1200. 1100. 1000 900. 800. 700. 600. 500. 400. 1500. 300. 1600. 200. 500. NS [arcsec]. 1700. 0. 100. 1800. 00. 3500. 1900. -500 3400. 2000. 2100. -1000. 3300. 2200. 3200 2300. 2400. 2500. 2600. -1000. 1400. 1000. 1300. 2700. 2800. 2900. 3000. 0 EW [arcsec]. 1200. 1100. 1000 900. 3100. 1000. 800. 700. 600. 500. 400. 1500. 300. 1600. 200. 500. NS [arcsec]. 1700. 0. 100. Emission Measure Peak Temperature. 1800. 00. 3500. 1900. 1.5. -500. 3.5 MK 3400. 2000. -1000. 2100. 3300. 2200. 3200 2300. -1000. 2400. 2500. 2600. 2700. 2800. 0 EW [arcsec]. 2900. 3000. 3100. 1000. . Figure 2: Top: A composite and large field-of-view soft X-ray (Al.1) map from Yohkoh/SXT.
(3) . with subdivision into 36 radial sectors, each wide. The circles indicate altitude levels of solar radii. Note two active regions at the east and west, a coronal streamer in the southeast, and coronal holes in the north and south. Bottom: Coronal temperature maps are shown for the 36 sectors of the same Yohkoh image. The peak temperature of the fitted differential emission measure distributions according to the multi-hydrostatic model defined in Eq.(3.3.7) (Aschwanden & Acton 2001).. . .
(4) 3. EIT 171 A -0.04. -0.06. deg. -0.08. -0.10. -0.12. -0.14. -0.16. 96/ 8/30 0:20:14.881 -0.05. 0.00. 0.05. 0.00 deg. 0.05. EIT 171 A filtered -0.04. -0.06. deg. -0.08. -0.10. -0.12. -0.14. -0.16. 96/ 8/30 0:20:14.881 -0.05. . Figure 3: SoHO/EIT Fe IX/X image of active region AR 7986, recorded on 1996-Aug-30,. ˚ sensitive in the temperature range of 0020:14 UT, at a wavelength of 171 A, MK (top). The greyscales of the image is scaled logarithmically in flux, the contours correspond to increments of 100 DN (data numbers). The heliographic grid has a spacing of . The filtered image (lower panel) was created by subtracting a smoothed image (using a boxcar of 3 3 pixels) from the original image, in order to enhance the loop fine structure (Aschwanden et al. 1999)..
(5) 4. Figure 4: 3-dimensional view of magnetic potential field lines (yellow lines) calculated with the Sakurai code by extrapolation of a SoHO/MDI magnetogram recorded on 1996 August 30, 20:48 ˚ loop segments (blue lines), UT (red surface with white and black polarities), the traced 171 A ˚ loop segments (green lines), and the traced 284 A ˚ loop segments (red lines). the traced 195 A The three views are: from vertical (top panel), from south (middle panel), and from east (bottom panel). The 3D coordinates of the traced EIT loops are based on stereoscopic reconstruction. Note some significant deviations between the observed loops and the theoretical magnetic field model (Aschwanden et al. 2000b)..
(6) 5. Figure 5: A 3D magnetic field represenation is rendered from photospheric magnetograms (optical image in orange), from extrapolated magnetic field lines (black lines), and the iso-gauss contours for thress gyroresonant layers that correspond to gyrofrequencies of 5 GHz (green), 8 GHz (blue), and 11 GHz (yellow). The outer contours of each igo-gauss surface demarcate the extent of radio emission at each frequency (Stephen White and Jeong-Woo Lee)..
(7) 6. Figure 6: (a) The small-scale magnetic field connects the network on the spatial scale of supergranulation cells, while large-scale magnetic fields extend up into the corona. This magnetic field extrapolation was computed based on a magnetogram recorded by SoHO/MDI on 1996 Oct 19. The tangled small-scale fields at the bottom of the corona have also been dubbed “magnetic carpet”. (b) Horizontal view of the same 3D representation of magnetic fields as in (a) (Neal Hurlburt and Karel Schrijver)..
(8) 7. Figure 7: A stack plot of a sunspot magnetogram in white light (bottom level), magnetic field strength (second level), vector field [kG] (third level), with an enlargment of the central sunspot (forth level) of active region NOAA 7722, recorded with the Advanced Stokes Polarimeter on 1994 May 17, 16:05 UT (Bruce Lites)..
(9) 8. Figure 8: Three-dimensional structure of magnetic field lines (red), isosurface of magnetic field (grey) and velocity vectors (green) of an emerging twisted fluxtube, calculated with a 3D MHD code. The bottom panel shows the projection of magnetic field lines onto the XY-plane. The emergence into the corona leads to a kinked alignment of solar active regions (Matsumoto et al. 1998)..
(10) 9. -200. TRACE 171 A. -300. 16. arcsec. 2. C4 C4 -400. C3 C3. C2 C2. 5. C1 C1. 7 83. 4. 9 -500. 1998-07-14 12:55:16.000 -400. -300 arcsec. -200. Figure 9: A TRACE 171 A˚ image is shown at the beginning of the flare 98-Jul-14, 12:55:16 UT, during which the first kink-mode oscillations were discovered. Kernels of flare emission are located at , which seem to trigger loop oscillations. The diagonal pattern across the brightness maximum at is a diffraction effect of the telescope. The analyzed loops are outlined with thin lines. Loops #4 and #6-9 show pronounced oscillations (Aschwanden et al. 1999b)..
(11) 10. Figure 10: Connectivity domains of a potential magnetic field are visualized by domains with different colors (bottom left). The logarithm of the magnetic field strength is shown with a colored contour map, with nullpoints marked as small white squares and separators are marked with black lines (top left). Fan and spine field lines from different perspectives are shown in the right frames. This numerical computation illustrates that most of the low-lying field lines are closed (in the transition region), while only a small fraction of the field lines are open and connect upward to the corona (Schrijver & Title 2002)..
(12) 11. Figure 11: TRACE image of the quiet Sun corona, taken in the 171 A˚ passband, on 1998Jun-10, 20:40 UT. The exposure time is 262 s, centered at (-122, -16) arcsec relative to disk center, displayed with a pixel resolution of 1”. Superimposed is a threshold SOHO/MDI full-disk magnetogram (with gree and red indicating the opposite polarities), taken at 20:48 UT, aligned within an arcsec. The color scale saturates at Mx cm , the magnetogram resolution is 1.4”. Note the detailed correspondence of small magnetic bipoles at the footpoints of coronal nanoflares and large-scale loops (Schrijver & Title 2002).. . . .
(13) 12. Figure 12: Numerical simulation of 3D separator reconnection. Yellow vectors (bottom right frame) indicate the driving pattern at the top boundary. The two reddish isosurfaces show the locations of the nullpoints and the purple isosurfaces the locations of strong current. Red and yellow field lines show the magnetic topology and the two nulls. The green and blue field lines provide the current topology. The bottom right frame is rotated by 180 degrees around the vertical axis. Note that the currents spread along the separators and enable reconnection along the entire separator lines (Galsgaard, Reddy, & Rickard 1997b)..
(14) 13. Figure 13: A 3D nullpoint with its associated spine field lines and fan surface is inferred for. . the first Bastille-day (1998-Jul-14, 12:55 UT) flare by Aulanier et al. (2000). Top: The magnetic field (with contours at G) from a KPNO magnetogram is ˚ image with a FOV of 203 104 Mm. The neutral lines are indicated overlaid on a TRACE 171 A with thick black lines. Middle: Extrapolated magnetic field lines are shown that closely trace out a fan-like separatrix surface above the -spot (P1-N1) and end in a 3D nullpoint (P2), which is connected through spine field lines to the leading polarity in the west (N2). Bottom: A 3D view is shown from a different viewing angle (from north-west) (Aulanier et al. 2000).. .
(15) 14 1999-Mar-18 16:40 UT, Yohkoh/SXT. 2000-Jun-07 14:49 UT, Yohkoh/SXT. 2001-Apr-19 13:31:05 UT, TRACE 171 A. 1998-Sep-30 14:30:05 UT, TRACE 171 A. 2000-07-14 10:59:32, TRACE 171 A. Figure 14: Soft X-ray and EUV images of flare loops and flare arcades with bipolar structure are shown. Yohkoh/SXT observed flares (1999-Mar-18, 16:40 UT, and 2000-Jun-07, 14:49 UT)with “candle-flame”-like cusp geometry during ongoing reconnection, while TRACE sees postflare loops once they cooled down to 1-2 MK, when they already relaxed into a near-dipolar state. Examples are shown for a small flare (2001-Apr-19 flare, 13:31 UT, GOES class M2), and for two large flares with long arcades, seen at the limb (1998-Sep-30, 14:30 UT) and on the disk (2000-Jul-14, 10:59 UT,X5.7 flare) (Aschwanden 2002b)..
(16) 15. 13/01/92 17:28:07 UT. 19/11/91 09:29:37 UT. ACC. ACC Color: SXT Cont: HXT/M1. Color: SXT Cont: HXT/M1. 17/02/93 10:35:36 UT. 04/10/92 22:17:06 UT. ACC ACC. Color: SXT Cont: HXT/M1. Color: HXT/Lo Cont: HXT/M1. Figure 15: The geometry of the acceleration region inferred from direct detections of above-theloop-top hard X-ray sources with Yohkoh/HXT (contours) and simultaneous modeling of electron time-of-flight distances based on energy-dependent time delays of 20-200 keV hard X-ray emission measured with BATSE/CGRO (crosses marked with ACC). Soft X-rays detected with Yohkoh/SXT or thermal hard X-ray emission from the low-energy channel of Yohkoh/HXT/Lo is shown in colors, outlining the flare loops (Aschwanden 1999b)..
(17) 16. Figure 16: A dynamic spectrum of flare/CME-related radio bursts, recorded on 1998-Aug24 with the Culgoora radiospectrograph (18-1000 MHz) and the WAVES radio detector on the WIND spacecraft (1-10 MHz). The composite dynamic spectrum shows type III bursts at the beginning and a slower-drifting type II burst later on. The frequency axis is shown with increasing frequency in y-direction, so that electron beams propagating from the Sun away drift in negative y-direction ( ) (Courtesy of Culgoora Observatory and Wind/WAVES team).. . .
(18) 17. ˚ on 2000-Nov-09, 05:03 UT, Figure 17: A postflare loop system is imaged with TRACE 171 A, some 6 hours after a GOES-class M7.4 flare on 2000-Nov-08, 22:42 UT in AR 9213 near the west limb. The flare was accompanied by a coronal mass ejection, observed by SoHO/LASCO. Note the numerous postflare loops which indicate continuous heating over more than 6 hours after the impulsive flare phase..
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