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ON THE RELATION BETWEEN FILAMENT ERUPTIONS, FLARES, AND CORONAL MASS EJECTIONS

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

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  1. 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

  2. 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.

  3. 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

  4. 3. Methods • Identifying a filament disappearance first. • Then they evaluate other observations to establish a relationship between the filament eruption and other phenomena.

  5. 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.

  6. 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.

  7. 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.

  8. 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).

  9. 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

  10. 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

  11. 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.

  12. 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.

  13. 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.

  14. Table1 -1-

  15. Table1 -2-

  16. Table1 -3-

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