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ON THE RELATION BETWEEN FILAMENT ERUPTIONS, FLARES, AND CORONAL MASS EJECTIONS Ju Jing, Vasyl B. Yurchyshyn, Guo Yang, Yan Xu, and Haimin Wang The Astrophysical Journal, 614:1054 1062, 2004 October 20. 太陽雑誌会速報 2005.2.28 殿岡 英顕. 1. Introduction.
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ON THE RELATION BETWEEN FILAMENT ERUPTIONS, FLARES, AND CORONAL MASS EJECTIONS Ju Jing, Vasyl B. Yurchyshyn, Guo Yang, Yan Xu, and Haimin Wang The Astrophysical Journal, 614:1054 1062, 2004 October 20 太陽雑誌会速報 2005.2.28 殿岡 英顕
1. Introduction • Early manifestations of CMEs in the solar atmosphere. • To find possible relation ships between solar surface phenomena such as filament eruptions and flares, the CMEs occurrence, and the properties of the associated magnetic field.
2. Data Sets • BBSO Hα full disk image • Kanzelehohe Solar Observatory full disk image • MDI magnetograms • EIT images • LASCO C2 coronagraphs • GOES Soft X-ray light curves • SGD event reports
3. Methods • Identifying a filament disappearance first. • Then they evaluate other observations to establish a relationship between the filament eruption and other phenomena.
3. Methods 3.1 Data Selection • Automatic filament disappearance detection program: 3620 events during 1999 Jun. 1 to 2003 Dec. 31. ->“filament disappearance report” • Surface area of at least 2000 arcsec^2 -> 243 events • Exclude misidentifications. • Add active region filament eruptions. <2000 arcsec^2 small events. 22 events. • Then total 106 events:43 complete Ha coverage.
3. Methods 3.2 Event Classification • Flares --- Flares were identified first.Then GOES and SGD were examined. • New flux emergence --- New flux emergences from MDI magnetograms. • CMEs --- LASCO C2 coronagraph images and the CME catalog to determine.The latitude of the CME be within +/- 30 deg.The CME appear within 2hr after eruption.
4. Results of filament eruption association • Type – Active region filament or quiescent filament. • Chirality --- When viewed from the positive polarity side, the axial field of a dextral filament points to the right. Sinistral to the left. • Emerging flux regions --- < 0.6 Rsun. “limb” for >0.6 Rsun. • Flares --- Ha, EIT, GOES X-ray plot, SGD. • CMEs --- LASCO C2.
5. DISCUSSION 5.1. Chirality • Filaments in the northern hemisphere are predominantly dextral, while filaments in the southern hemisphere are sinistral. • Filament chirality and the sign of magnetic helicity in interplanetary CMEs (ICMEs).
5. DISCUSSION 5.2. New Flux Emergence KSO BBSO • 80 events. • 54 (68%) events by new flux emergence within 15 hr prior to the filament eruption. • Both active and quiet-Sun regions. MDI
5. DISCUSSION 5.3. Flares and CMEs -1- • Top panel .. the heliographic latitude of flares and CMEs. • 55 (56%) of 98 events were accompanied by CMEs. • 94% by Gilbert et al (2000)83% by Gopalswamy et al.(2003)10%-30% range by Yang & Wang (2002) • Bottom panel .. the distribution of eruptive filaments as a function of distance from the solar disk center. • 70% occurs in R=0.4-0.6Rsun
5. DISCUSSION 5.3. Flares and CMEs -2- • Active region filaments (ARF) v.s. Quiescent filaments (QF). • Association with flares: ARF (95%), QF (28%) • 85QFs: 46(54%) with CMEs, 23(27%) with flares.
5. DISCUSSION 5.4. Halo CMEs • 7 eruptive filament associated with halo CMEs and Geomagnetic Storms. • The orientation of CMEs are assumed to be the same as the orientationof the axial magnetic field of the filaments.
6. SUMMARY • 106 major filament eruption events from 1999 Jan 1 to 2003 Dec 31. • 55(56%) of 98 events were associated with CMEs. • Active region filament eruptins have a considarably higher flare association(95%) than quiesent filament eruption (27%) • 54(68%) of 80 disk events were associated with new flux emergence. • The chirality and the orientation of magnetic fields of halo CMEs.