Magnetic properties of flare-CME productive  active regions and CME speed

Guo, J.; Zhang, H. Q.; Chumak, O. V.

doi:10.1051/0004-6361:20065888

Cited by 25 publications

(16 citation statements)

References 29 publications

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“…This parameter could roughly quantify the magnetic complexity of active regions. Our previous (Guo et al 2006, 2007; Guo & Zhang 2007) studies have confirmed that the higher d E , the more complex the magnetic field of the ARs. In the same way as in the previous work, we choose a threshold of 100 G to measure d E for the ARs from MDI synoptic charts.…”

Section: Methodssupporting

confidence: 59%

“…It has been pointed out that this parameter could describe the degree of isolation or mutual penetration of the two polarities of an AR quantitatively. Recently, using the Solar and Heliospheric Observatory (SOHO) Michelson Doppler Imager (MDI) line‐of sight magnetograms, we have carried out a systemic investigation of the quantitative study of the magnetic complexity of ARs with this parameter (named effective distance, d E , in our work: Guo & Zhang 2007; Guo, Zhang & Chumak 2007). We have carried out a statistical analysis with a large sample of 848 ARs and confirmed the basic agreement between the value of d E and MWMC.…”

Section: Introductionmentioning

confidence: 99%

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The evolution of the quantified magnetic complexity of active regions in the 23rd solar cycle

Guo¹,

Zhang²,

Chumak³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present a statistical study to show how the quantified magnetic complexity of active regions (ARs) evolves in the 23rd solar cycle. We collect a sample of 1039 ARs in the period 1996–2008 based on magnetic synoptic charts from the Solar and Heliospheric Observatory Michelson Doppler Imager (SOHO/MDI) and National Solar Observatory (NSO/Kitt Peak). A structural parameter dE is used to quantify the magnetic complexity of ARs. We have found that the yearly mean magnetic complexity of ARs is high near the solar maximum and low near the solar minimum. The deviation of the yearly mean dE of the ARs at the solar maximum from that at the solar minimum is about 59.8 per cent for the rising phase and 38.1 per cent for the declining phase. Most ARs are relatively simple and bipolar, even at the solar maximum. The yearly ratio of the number of complex ARs with dE greater than 1 to the number of total ARs increases rapidly and persistently in the rising phase of the solar cycle, but decreases with large fluctuations in the declining phase. By studying the distribution of ARs of different complex degree over the sunspot butterfly diagram, it is found that complex ARs are scattered over the 23rd solar cycle and there is some asymmetry in the northern and southern hemispheres.

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Section: Methodssupporting

confidence: 59%

Section: Introductionmentioning

confidence: 99%

The evolution of the quantified magnetic complexity of active regions in the 23rd solar cycle

Guo¹,

Zhang²,

Chumak³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…Through examining 117 ARs, Canfield et al [1999] found that ARs are more likely to be eruptive if they are either sigmoidal or large. Guo et al [2007] investigated 55 flare‐CME productive ARs and found that fast CMEs tended to initiate in ARs with large magnetic flux or long lengths of main polarity inversion lines (PILs). Through investigating 57 fastest CMEs with speed larger than 1500 km s −1 from 1996 June to 2007 January as well as 1143 ARs recognized from magnetic synoptic charts obtained by Michelson Doppler Imager (MDI) on board Solar and Heliospheric Observatory (SOHO), Wang and Zhang [2008] found that there was a general trend that a larger, stronger, and more complex AR was more likely to produce a faster CME.…”

Section: Introductionmentioning

confidence: 99%

Statistical study of coronal mass ejection source locations: 2. Role of active regions in CME production

Chen¹,

Wang²,

Shen³

et al. 2011

J. Geophys. Res.

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.[1] This is the second paper of the statistical study of coronal mass ejection (CME) source locations, in which the relationship between CMEs and active regions (ARs) is statistically studied on the basis of the information of CME source locations and the ARs automatically extracted from magnetic synoptic charts of Michelson Doppler Imager (MDI) during 1997-1998. Totally, 224 CMEs with a known location and 108 MDI ARs are included in our sample. It is found that about 63% of the CMEs are related with ARs, at least about 53% of the ARs produced one or more CMEs, and particularly about 14% of ARs are CME-rich (3 or more CMEs were generated) during one transit across the visible disk. Several issues are then tried to clarify: whether or not the CMEs originating from ARs are distinct from others, whether or not the CME kinematics depend on AR properties, and whether or not the CME productivity depends on AR properties. The statistical results suggest that (1) there is no evident difference between AR-related and non-AR-related CMEs in terms of CME speed, acceleration and width, (2) the size, strength and complexity of ARs do little with the kinematic properties of CMEs, but have significant effects on the CME productivity, and (3) the sunspots in all the most productive ARs at least belong to bg type, whereas 90% of those in CME-less ARs are a or b type only. A detailed analysis on CME-rich ARs further reveals that (1) the distribution of the waiting time of same-AR CMEs, consists of two parts with a separation at about 15 hours, which implies that the CMEs with a waiting time shorter than 15 hours are probably truly physical related, and (2) an AR tends to produce such related same-AR CMEs at a pace of 8 hours, but cannot produce two or more fast CMEs (>800 km s À1) within a time interval of 15 hours. This interesting phenomenon is particularly discussed.

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“…Statistical studies show that there are close relationships between CMEs and active regions (ARs, Subramanian & Dere, 20 Zhou et al, 19 Guo et al, 21,22 Chen et al 23 ) and AR magnetic non-potentiality (Falconer et al, 24 Schmieder 25 ). However, the related-ARs do little effects on the kinematic properties of CMEs, except for the CME productivity (Chen et al 23 ).…”

Section: Cme-related Surface Activitymentioning

confidence: 99%

“…The eruption processes of flares/CMEs are well studied by many authors (e. g., Zhang et al, 26 Lin, 27 Guo et al, 22 and Wang & Zhang 28 ). In Zhou et al, 19 it is found that all the earth-directed halo CMEs were accompanied by the local brightening in EUV and/or Ha wavebands.…”

Section: Cme-related Surface Activitymentioning

confidence: 99%

The Source Regions of Coronal Mass Ejections

Zhou

2013

Int. J. Mod. Phys. Conf. Ser.

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Coronal Mass Ejection is an entire process leading to the ejection of mass and magnetic flux into interplanetary space. Its source is studied by analyzing the associated surface activity. Analysis results show that CMEs have large-scale magnetic source structures, which provide their energy, initiation, and final angular width. This paper review the studies of CME source regions with laying emphasis on their large-scale source structures.

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Magnetic properties of flare-CME productive active regions and CME speed

Cited by 25 publications

References 29 publications

The evolution of the quantified magnetic complexity of active regions in the 23rd solar cycle

The evolution of the quantified magnetic complexity of active regions in the 23rd solar cycle

Statistical study of coronal mass ejection source locations: 2. Role of active regions in CME production

The Source Regions of Coronal Mass Ejections

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