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2 Typeset by L A TEX 2ε at March 16, 2007 With package CASthesis v0.1g of CTEX.ORG

3 A Quantitative Study on Magnetic Field of Solar Active Regions and Flare-Coronal-Mass-Ejections Juan Guo Supervisor: Prof. Hong-Qi Zhang National Astronomical Observatories Chinese Academy of Sciences March, 2007 Submitted in total fulfilment of the requirements for the degree of Ph.D. in Solar Physics Research

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5 CME d E F t T ilt Lsg CME 1. d E 24 9 β d E 1 2 βδ d E 1 9 βγδ 8 d E 1 4 βγ 1 d E 1 3 d E 1 d E d E d E d E 2. d E F t T ilt d E δ δ d E δ d E

6 d E 0.81 F t 0.50 T ilt CME CME d E F t T ilt Lsg CME CME CME F t d E d E CME CME CME d E Lsg F t F t Lsg T ilt 86 CME 11 CME Km/s CME β CME Lsg 50 Lsg CME Lsg CME CME CME

7 Abstract Magnetic field plays a central role in solar activities. Most intense flares and fast coronal-mass-ejections (CMEs) initiate in active regions with complex configuration. It is helpful for prediction of solar activities to quantify the complexity of magnetic field of active regions properly. Using some space-borne observations, we quantify the magnetic structure with effective distance d E and put forward the quantitative classification for magnetic field of solar active regions based on d E. Then using d E, together with other parameters (total flux (F t), tilt angle (T ilt), length of strong field and strong gradient main neutral line (Lsg)), we have carried out some quantitative studies, including studies on evolutions of magnetic field of solar active regions, on the statistical relationship between magnetic properties of solar active regions and flare-index or CME speed, etc. Our main contributions are as follows: 1. Quantitative classification for magnetic field of solar active regions. Magnetograms of 24 active regions of different types with MWMC has been studied. It has been found that all the 9 β regions show effective distance (d E ) less than unity; both of the 2 βδ regions show d E more than unity; 8 out of 9 βγδ regions show d E more than unity; for the 4 βγ regions, there are some discrepancies: 1 region shows d E more than unity, while 3 regions show d E less than unity. These indicate the more complex the active regions, the higher the value of d E. So there is a basic agreement between MWMC and d E. Moreover, d E could quantify the magnetic configuration of active regions. 2. Quantitative study on evolution of solar active regions. Evolutions of

8 8 - magnetic fields of five active regions have been studied quantitatively with d E, F t and T ilt. It has been found that the evolution of magnetic fields can be described in three aspects quantitatively and accurately by the three parameters, in particular d E on the analysis of δ-type active regions: d E increases for active regions with developing δ structure, while d E decreases for active regions with decaying δ structure. 3. Statistical correlation between properties of magnetic field of solar active regions and flare-index. 43 flare-associated active regions have been studied to investigate and quantify the statistical correlation between flare-index and each of the three parameters d E, F t and T ilt. The linear correlation coefficients are 0.81, 0.50, 0.01 respectively. 4. Statistical correlation between properties of magnetic field of solar active regions and CME speed. A sample of 86 flare-cmes originated in 55 solar active regions near the central meridian has been collected. This sample includes most of the important flare-cmes initiating in active regions located near the central meridian in the interval from 1997 to Four measures, including d E, F t, T ilt and Lsg, are used to quantify the properties of the magnetic field of flare- CME productive active regions. It has been found that for CMEs initiating in active regions, fast CMEs tend to initiate in active regions with large F t or large d E among the four parameters, d E correlates with CME speed best; In flareassociated CMEs, faster CMEs tend to be accompanied by more intense flares, the linear correlation coefficient is 0.58; The parameters d E, Lsg and F t correlate with one another well, especially F t and Lsg, while T ilt correlates with other parameters weakly; For the 86 CMEs initiating in active regions, The occurrence of 11 slow CMEs and 1 fast CME in β type regions with Lsg far below the threshold of 50 arcsec reminds us of some exceptions to be considered when Lsg

9 ABSTRACT 9 with the threshold is used to predict the CME productivity of active regions. We arrange the thesis as follows: A brief introduction is presented in Chapter 1. Our main work are presented in Chapter 2 and Chapter 3. The summary of our work and prospects are given in the last chapter. Keywords: solar activity, magnetic field, flare, coronal mass ejection (CME)

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11 5 Abstract CME δ

12 F t T ilt d E d E β NOAA βδ NOAA βγδ NOAA βγδ NOAA βγδ NOAA CME CME CME Lsg

13 d E Lsg CME CME CME

14

15 1.1

16 [ 2000] 1 ± K 5500 K G 4 Evershed

17 Spuror Hale-Nicholson Maunder Wilson 1919 Wilson Wilson α β γ 1960 δ α p AP α f AF β p BP β f BF

18 4 - β B β γ Br β γ r δ D 2 [ 2000] Zurich 1.1: Zurich [Waldmeier 1947]

19 5 Zurich 1.1 A B C D E F G J A B C D 10 E 10 F 15 G 10 H 2.5 J 2.5 Zurich Wilson McIntoch McIntoch 1.2 Zurich Zurich McIntoch

20 6-1.2: McIntoch [McIntosh 1990] Zurich 9 7 A B C D E F H G J G E F J H G

21 7 J J H 6 x 3 r s a 2.5 a h s 2.5 k a γ k 4 x individual o open

22 8 - i intermediate c compact Zurich G Ero Fro Eso Fso Eao Fao Eho Fho Eko Fko J Hrx Hsx Hax Carrington Hodgson Hα Hα 1 Å γ X 10 3 ev ev erg GOES Geostationary Operational Environmental Satellites X B C M X X 1.1

23 9 1.1: X Peak Flux Range ( nm) Classification mks system (W m 2 ) cgs system (erg cm 2 s 1 ) A Φ < 10 7 Φ < 10 4 B 10 7 < Φ < < Φ < 10 3 C 10 6 < Φ < < Φ < 10 2 M 10 5 < Φ < < Φ < 10 1 X 10 4 < Φ 10 1 < Φ CME CME OSO-7 Orbiting Solar Observatory CME 1973 Skylab CME SMM Solar Maximum Mission SOHO Solar and Heliospheric Observatory CME CME CME CME CME CME 360 CME CME ±50 CME 10 km/s 2000 km/s 450 km/s CME g g

24 erg Gosling [1993] CME CME CME CME CME CME [Krall et al Tanaka 1991] [Low and Nakagawa 1975 Sakurai 1993]

25 Zirin and Tanaka [1973] Hα δ Hagyard et al. [1984] δ 85 X Tanaka [1991] δ 4300 δ Zirin and Wang [1993] 6 δ 5 δ 6 δ 3980 δ Yohkoh X Canfield [1999] S S S S

26 12 - CME S S S S Yohkoh X Falconer et al. [ ] X X CME [Falconer et al. 2003] Hα Severny and Bumba [1958] Moreten and Severny [1968] 30 80% Hα Li et al. [1999] NOAA AR

27 13 4 δ 1 2 Zhang [2001b] J z = B µ 0 ( by x - bx y ) + 1 µ 0 (b y B x b x B y ) h m = A B A B B = A B = 0 V H m = h m dv h c = B ( B) B J = 1 µ 0 ( B) J = 0 V H c = h c dv h c Bao and Zhang [1999] Hβ

28 14 - a. b. 1.3: a NOAA 7321 ± b ± G 2 m 1 [Zhang 2001a] Zhang et al. [2000] 1992 NOAA 7070 X 1 X 2

29 15 a. b. 1.4: a NOAA b [Zhang 2001a] X δ Zhang [2001] 1 α 2 X

30 : NOAA 9077 [Deng et al. 2001] Deng et al. [2001] NOAA

31 Liu and Zhang [2002] -CME NOAA 9077 δ 2 δ F4 δ δ Seehafer [1990] α 16 Pevtsov et al. [1995] α 69 75% 69% Bao and Zhang [1998] % 81% Bao et al. [2002]

32 18-1.6: TRACE 5000 NOAA P1 P2 F F4 P6 δ P F [Liu and Zhang 2002] [Zhang and Bao ] Tian et al. [2001]

33 19 1.7: 3 ± / P6 F F4 [Liu and Zhang 2002] B B 1 60% 2 M Tian et al. [2002a] % 68% 84% δ

34 20 - a. b. 1.8: a 18 NOAA hc F4 P6 P6-F4 δ b [Liu and Zhang 2002] Tanaka and Nakagawa [1983]

35 21 Herdiwijaya et al. [1997] % liu and Zhang [2001] NOAA 9077 δ NOAA B/X5.7 βγδ Ishii et al. [ ] δ NOAA 4201 NOAA 5395 βγδ Kurokawa et al. [2002] NOAA 9026 δ

36 : I a T1 T2 T3 T1 b [Kurokawa et al. 2002]

37 : II a b c d e f e [Kurokawa et al. 2002] Wang [1995] Wang and Wang [1996] Hα Hβ Wang et al. [1999]

38 24 - X δ α β βγ γ 1960 Kunzel [1960] δ δ Warwick [1966] δ δ δ Tanaka [1980] δ 90% δ Sammis et al. [2000] 8 βγδ 40% CME Hα Hα 90% CME [Munro et al. 1979] SMM 151 CME Harrison [1995] CME NOAA 9026 NOAA

39 NOAA [Liu and Zhang, Deng et al Tian et al. 2002a 2002b 2003 Zhang 2001a Zhang et al Zhang 2004] δ CME δ 1.4

40

41 Wilson δ δ Chumak and Chumak [1987] CME 2.2 SOHO/MDI CCD MDI MDI < l < +45 Chae et al. [2001]

42 28-100G SEC http : // SOHO/LASCO/CME http : //cdaw.gsfc.nasa.gov/cme list/index.html CME Tian et al. [2003] Zhou et al. [2003] CME F t [Giovanelli 1939 McIntosh 1990 Canfield et al Tian et al. 2002a] F t = F s + F n (2.1) Fs Fn T ilt Ω [Parker 1955]

43 29 [Hale et al D Silva and Choudhuri 1993 Fan et al Fisher et al Longcope and Fisher 1996 Nandy and Choudhuri 2001 Wang and Sheeley 2003 Holder et al. 2004] [Tian et al. 1999] X s = (B si X si )/ B si (2.2) Y s = (B si Y si )/ B si (2.3) X n = (B ni X ni )/ B ni (2.4) Y n = (B ni Y ni )/ B ni (2.5) tan(t ilt) = δy/δx (2.6) δy δx d E Chumak and Chumak [1987] Kononvich et al. [1999] Chumak and Zhang [2003] Chumak et al. [2004] 50

44 30-2.1: 23 T ilt N S d E d E d E d E 100 d E d E d E = (Rn + Rs)/Rsn (2.7) Rs = (Ns/π) 1/2 (2.8) Rn = (Nn/π) 1/2 (2.9) Ns Nn Rsn

45 d E 2.2 a d E 1 β 2.2 b d E 1 δ d E 2.4 d E β 1 2 βδ 1 9 βγδ βγ 2.2: d E a d E 1 b d E 1

46 d E d E d E d E CME d E β βδ βγδ βγδ βγδ β NOAA NOAA β 2.3 β 2.8 d E

47 33 2.1: 24 d E NOAA Date Location Mag. class d E Oct 1997 N16W14 β Feb 2000 S29W11 β Dec 2000 N14W06 β Mar 2001 N08W07 β Apr 2001 S06W04 β Apr 2001 N08W06 β Jul 2002 N12W13 β Jul 2002 S07W06 β Feb 2004 N14W09 β Nov 1997 S19W12 βγ May 1998 S17W22 βγ Nov 1999 N10W07 βγ Mar 2003 S13W14 βγ Sep 2000 N14E01 βδ Jan 2005 N13W03 βδ Jun 2000 N20E03 βγδ Jul 2000 N18W09 βγδ Mar 2001 N17W18 βγδ Apr 2001 S21E05 βγδ Sep 2001 S19W08 βγδ Jul 2002 N18W00 βγδ Oct 2003 N04W00 βγδ Oct 2003 S17E04 βγδ Oct 2003 N08W04 βγδ

48 βδ NOAA NOAA βδ β βδ : β NOAA N S

49 35 d E T ilt F t 3 X :00 UT X :25 UT X :59 UT X3.8 d E F t T ilt βγδ NOAA NOAA βγδ [Zhang et al Liu and Zhang 2006] β F1 P1 P2 F2 P1 F1 β βγδ P2 F2 P2 F1 P2 P2 F1 P2 F1 δ βγδ [Zirin and Liggett 1987] P1 F1 δ δ N S d E 0.9 d E 1.88 T ilt

50 36-2.4: βδ NOAA N S

51 βγδ NOAA NOAA βγδ P1 P2 P1 2.5: βγδ NOAA N S P1 P2 F1 F2

52 38 - P2 P3 P1 P2 P3 2.8 d E S P2 N 2.8 T ilt F t :21 UT X1.2 T ilt d E βγδ NOAA 9026 NOAA 9026 [Kurokawa et al Zhang 2004 Wang et al. 2004] δ βγδ βγ 2.8 d E δ 2.8 T ilt X :00 UT X :58 UT X :34 UT X1.2

53 39 2.6: βγδ NOAA N S P1 P2 P3

54 40-2.7: βγδ NOAA N S 01:36:30 UT P

55 41 2.8: T ilt d E F t X d E 1 T ilt F t 2.6 Sammis [2000] βγδ d E 43

56 X M C X 10 4 W m d E Sammis [2000] d E 2.7 CME CME CME [Munro et al Webb and Hundhausen 1987 Gilbert et al Zhou et al. 2003] CME CME CME CME 1 MDI d E F t T ilt

57 CME CME d E F t T ilt d E CME 0.64 CME CME d E CME 2.9:

58 44 - d E F t CME 0.39 T ilt CME : CME

59 NOAA 9026 Falconer et al. [ ] CME Tian and Liu [2003] CME 2.7 Zhang [2004] T ilt NOAA 9026 P δ [Kurokawa et al. 2002] Shi and Wang [1993] 95% X δ 282 δ 23% X δ 19 X X δ Shi and Wang [1993] δ X X X Shi and Wang [1993]

60 46 - β βγ d E 2.9 Chumak and Chumak [1987] d E d E d E F t T ilt CME 1 24 d E d E d E CME 2 d E F t T ilt d E δ δ d E δ d E 3 43 F t T ilt d E d E

61 47 Sammis [2000] CME F t T ilt d E CME CME d E d E CME

62

63 - CME CME 3.1 CME CME CME CME [Zhou et al. 2003] CME CME [Moore and LaBonte 1980 Moore et al Canfield et al. 1999] Falconer et al. [ ] 180 Zhang [2001b 2006a] NOAA 6659 Hahn et al. [2005] 29 Hα Wang et al. [2006] 5

64 50 - CME 17 Falconer et al. [2003] length of strong field and strong gradient main neutral line Lsg CME Lsg CME d E -CME 86 CME CME CME F t T ilt d E 100 G Lsg CME CME < l < +45 CME Tian et al. [2003] Zhou et al. [2003] Moon et al. [2005] CME CME SEC CME CME SOHO/MDI 96 Moon et al. [2002] 20

65 - CME CME Chae et al. [2001] 86 CME 3.3 Lsg [ Zirin and Liggett 1987 Zirin 1988 Hagyard and Rabin 1986 Hagyard 1988 Zhang et al Zhang 2001 ] Lsg Falconer et al. [2003] >150 G >50 G/Mm Lsg Falconer et al. [2003] Lsg CME CME Lsg Lsg Km 50 CME Lsg 150 G 50 G/Mm 1 Lsg Lsg

66 NOAA X3.8 06:59 UT 09:52 UT 10:07 UT 2547 Km/s CME CME SOHO/LASCO C2 09:54 UT :24 UT MDI 96 X NOAA T ilt d E S N 3.1 b-o N S c-o b-o-c T ilt d E S N δ SE + NF SN d E 3.55 β d E 1 d E d E NOAA : G

67 - CME CME : : LASCO/C :54 UT NOAA CME NOAA :24 UT N S b-o-c T ilt NOAA :24 UT d E N S S-E N-F S-N d E 3.55 NOAA :24 UT Lsg

68 54-50 G/Mm Lsg 523 Falconer et al. [2003] CME d E d E 3.5 CME NOAA βγ 5 1 βδ 5 2 βγδ d E β 20/24 d E 1 2 βδ γδ βγδ 18/20 d E 1 14 βγ 6 d E 1 8 d E 1 24 d E

69 - CME CME : CC P l CC Sr S Sr d E vs. F t e-8 d E vs. Lsg e-10 F t vs. Lsg e-22 T ilt vs. F t T ilt vs. d E T ilt vs. lsg Lsg CME 3.5 Lsg CME 74/86 Lsg Falconer et al. [2003] Lsg CME Lsg 50 4 CME Lsg 0 Lsg 50 CME 12 CME β 12 CME 11 CME CME 1000 Km/S T ilt F t d E Lsg Pearson s CC P l Spearman s CC Sr Spearman s S Sr S Sr 0.0

70 56-3.2:

71 - CME CME S Sr Spearman s F t d E Lsg F t Lsg F t d E Lsg CME 3.5 NOAA NOAA 9415 NOAA 9077 NOAA T ilt CME 17 CME T ilt d E Lsg NOAA T ilt CME NOAA F t d E Lsg X X28 19 M 8 CME CME 3.3 CME T ilt F t d E Lsg 3.2

72 58-3.3: CME

73 - CME CME : CME CC P l CC Sr S Sr CC P V CME vs. T ilt V CME vs. F t (d E ) (Lsg) V CME vs. Lsg (F t) (d E ) V CME vs. d E e (F t) (Lsg) CME T ilt Pearson s CC P l CME F t CME d E Pearson s CC P l d E CME T ilt F t CME F t CME d E Lsg d E CME Lsg CME d E d E δ d E CME 18 βγδ 8 βγ 2 βδ 3 β Lsg CME [Falconer et al. 2005] 3.2 Spearman s CC Sr Pearson s CC P l Spearman s S Sr d E CME S Sr S Sr S Sr

74 60 - Spearman s d E CME Spearman s Pearson s F t d E Lsg CME CME Lsg d E Lsg d E F t CME Lsg d E F t CC P F t CME d E F t F t CME Lsg F t 3.2 Pearson s Spearman s Pearson s Spearman s 3.2 CME F t Lsg d E CME d E Lsg F t Pearson s Spearman s CME d E F t CME

75 - CME CME 61 Lsg F t d E Pearson s Spearman s CME Lsg Pearson s Spearman s F t d E CME CME F t d E CME d E F t Spearman s S Sr CC P CME Lsg d E F t CME 3.3: CME CC P l CC Sr S Sr V CME vs. F t d E e-4 V CME vs. F t Lsg CME CME F t d E F t Lsg CME F t d E CME F t Lsg CME CME F t

76 62-3.4: CME d E Lsg CME F t d E Lsg NOAA CME F t Lsg NOAA CME F t d E CC P l = CC Sr = S Sr = 6.11e-8 CME F t Lsg CC P l = CC Sr = S Sr = 2.08e CME F t d E Lsg 6 CME

77 - CME CME 63 CME F t Lsg CME F t d E F t Lsg 3.5: CME X 3.4: CME X CC P l CC Sr S Sr V CME vs. I flare e CME 86 CME Km/s CME CME M X X CME 3.5 C M X Pearson s Spearman s CME Pearson s Spearman s Spearman s

78 e-11 Spearman s CME CME CME CME T ilt F t Ed Lsg 1 CME CME 2 CME CME 3 d E Lsg F t F t Lsg T ilt 4 86 CME 11 CME Km/s CME β CME Lsg 50 Lsg CME Lsg CME CME

79 - CME CME : 86 /CME Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 1997 Apr 07 14: :50 C6.8 S25E β Oct 21 18: :00 C3.3 N17E β Nov 03 11: :13 M1.4 S20W βγδ Nov 04 06: :52 X2.1 S14W βγδ Apr 29 16: :06 M6.8 S18E βγ May 01 23: :40 C2.6 S19W γδ May 02 05: :48 C5.4 S19W βγδ May 02 14: :31 X1.1 S15W βγδ May 03 22: :12 M1.4 S13W βγ Nov 04 07: :13 C1.6 N17E βγ May 03 06: :36 M4.4 N17E β May 10 05: :24 M2.5 N16E β Aug 07 23: :04 C3.9 S28E β

80 66-3.5: continued. Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 1999 Aug 17 13: :47 C2.6 N22E β Aug 28 18: :52 X1.1 S26W βγδ Sep 01 02: :56 c C2.7 N08W β Sep 13 17: :38 C2.6 N16W β Sep 13 09: :05 C4.9 N22E β Oct 14 09: :58 X1.8 N12E βγδ Nov 26 17: :40 C2.3 S12W β Jan 18 17: :10 M3.9 S19E β Jan 28 20: :45 C4.7 S31W β Feb 09 19: :26 C7.4 S14W β Feb 08 09: :43 M1.3 N25E βγ Feb 12 04: :10 M1.7 N26E βγ Feb 17 20: :45 M2.5 S25W βγ Feb 17 21: :19 M1.3 S29E β

81 - CME CME : continued. Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 2000 Apr 10 00: :29 c M3.1 S14E βγδ May 10 20: :32 C8.7 N14E β Jun 02 10: :04 C2.4 N10E β Jun 06 15: :06 X2.3 N20E βγδ Jun 07 16: :04 X1.2 N23W βγδ Jun 10 17: :37 M5.2 N22W β Jul 10 21: :05 M5.7 N17E βγδ Jul 14 10: :03 X5.7 N22W βγδ Jul 25 03: :47 M8.0 N06W βγ Aug 09 16: :33 C2.3 N11E βγ Sep 01 06: :42 C1.6 S20W β Sep 15 12: :54 C9.5 N13E βδ Sep 15 15: :31 M2.0 N12E βδ Sep 16 05: :07 M5.9 N14W βγ

82 68-3.5: continued. Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 2000 Oct 02 03: :47 C4.1 S09E βγ Oct 09 23: :22 C6.7 N01W β Nov 23 23: :18 M1.0 N22W β Nov 24 05: :55 X2.0 N20W βγ Nov 24 15: :51 X2.3 N22W βγ Nov 24 22: :43 X1.8 N21W βγ Nov 25 09: :06 M3.5 N18W βγ Nov 25 19: :33 X1.9 N20W βγ Nov 26 03: :47 M2.2 N19W βγ Nov 26 17: :34 X4.0 N18W βγ Dec 18 11: :03 C7.0 N15E β Jan 10 00: :34 C5.9 N13E βγ Jan 20 19: :40 M1.2 S07E βγ Mar 24 20: :37 M1.7 N15E β

83 - CME CME : continued. Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 2001 Mar 28 12: :21 M4.3 N18E βγδ Mar 28 19: :58 M1.5 N14W βγδ Mar 29 00: :25 c M2.1 N17W βγδ Mar 29 10: :57 X1.7 N17W βγδ Mar 29 14: :09 M1.6 N16W βγδ Apr 06 19: :10 X5.6 S24E βγ Apr 09 15: :20 M7.9 S21W βγδ Apr 10 05: :06 X2.3 S23W βγδ Apr 11 13: :56 M2.3 S22W βγδ Aug 25 16: :23 X5.3 S17E βγδ Sep 11 14: :16 C3.2 N14E β Sep 17 08: :18 M1.5 S14E βγ Sep 24 10: :32 X2.6 S16E βγδ Oct 19 01: :47 X1.6 N16W βγδ

84 70-3.5: continued. Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 2001 Oct 19 16: :13 X1.6 N15W βγδ Oct 22 15: :27 M6.7 S20E βγδ Oct 25 15: :42 X1.3 S16W βγδ Nov 01 22: :38 M1.1 N12W βγδ Nov 04 16: :03 X1.0 N06W βγδ Nov 17 05: :48 M2.8 S13E β Nov 22 23: :09 M9.9 S15W βγδ Nov 28 17: :32 M6.9 N04E βγδ Dec 11 08: :02 X2.8 N16E βγ Dec 13 14: :24 X6.2 N16E βγ Jul 15 20: :50 X3.0 N19W βγδ Aug 16 12: :32 M5.2 S14E βγδ Oct 28 11: :01 X17.2 S17E βγδ Oct 29 20: :37 X10 S15W βγδ

85 - CME CME : continued. Date Time a V b Flare X-Ray Position NOAA Mag. T ilt F t de Lsg (km s 1 ) Start Class (deg) Class (deg) (10 21 Mx) (arcsec) 2005 Jan 15 06: :56 M8.6 N11E βδ Jan 15 23: :54 X2.6 N14W βδ Jan 17 09: :59 X3.8 N13W βδ a CME LASCO C2 b CME c CME Lsg 50

86

87 Wilson Z rich McIntoch Wilson δ Chumak O. V CME 1 d E d E 2 5 d E F t T ilt d E δ δ d E δ d E 3 43 d E F t T ilt d E CME

88 74 - CME CME F t d E d E CME d E Lsg F t F t Lsg T ilt 86 CME 11 CME Km/s CME β CME Lsg 50 Lsg CME Lsg CME CME CME CME CME d E d E d E γ d E d E α

89 CME

90 76 太阳活动区磁场结构与耀斑-日冕物质抛射的定量研究 图 4.1: 全日面太阳光学和磁场监测系统望远镜 [Zhang 2006b]

91 77 4.2: ± [Zhang 2006b]

92 78-4.3: ± [Zhang 2006b]

93 第四章 总结与展望 图 4.4: 2006 年 4 月 22 日的全日面 Hα 图 [Zhang 2006b] 79

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