Relationship between CME velocities and X-ray fluxes of associated flares

An-qin, Chen; Zong, Weiguo

doi:10.1088/1674-4527/9/4/009

Cited by 16 publications

(13 citation statements)

References 16 publications

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“…The fastest CMEs are associated with the strongest flares. This relation has been presented by other authors (Moon et al, 2003;Burkepile et al, 2004;Maričič et al, 2007;Chen and Zong, 2009;Bein et al, 2012) and is also observed in our sample of events (Figure 2, left). It is worth noticing that CMEs connected with the slow LDEs are very fast.…”

Section: Resultssupporting

confidence: 92%

“…Relationships between flares and CMEs, e.g. SXR flux vs. CME velocity, duration of the flare rising phase vs. duration of the acceleration phase, were investigated by many authors (Zhang et al, 2001;Moon et al, 2003;Burkepile et al, 2004;Vršnak, Sudar, and Ruždjak, 2005;Maričič et al, 2007;Chen and Zong, 2009;Berkebile-Stoiser et al, 2012). Zhang et al (2001) investigated the temporal relationship between CMEs and associated solar flares.…”

Section: Introductionmentioning

confidence: 99%

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Coronal Mass Ejections Associated with Slow Long Duration Flares

2013

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It is well known that there is a temporal relationship between coronal mass ejections (CMEs) and associated flares. The duration of the acceleration phase is related to the duration of the rise phase of a flare. We investigate CMEs associated with slow long duration events (LDEs), i.e. flares with the long rising phase. We determined the relationships between flares and CMEs and analyzed the CME kinematics in detail. The parameters of the flares (GOES flux, duration of the rising phase) show strong correlations with the CME parameters (velocity, acceleration during main acceleration phase, and duration of the CME acceleration phase). These correlations confirm the strong relation between slow LDEs and CMEs. We also analyzed the relation between the parameters of the CMEs, i.e. a velocity, an acceleration during the main acceleration phase, a duration of the acceleration phase, and a height of a CME at the end of the acceleration phase. The CMEs associated with the slow LDEs are characterized by high velocity during the propagation phase, with the median equal to 1423 km s −1 . In half of the analyzed cases, the main acceleration was low (a < 300 m s −2 ), which suggests that the high velocity is caused by the prolonged acceleration phase (the median for the duration of the acceleration phase is equal 90 minutes). The CMEs were accelerated up to several solar radii (with the median ≈ 7 R ), which is much U. Bak-Stȩślicka is a visiting scientist at High Altitude Obsevatory, NCAR, Boulder, USA.U. Bak-Stȩślicka ( ) · S. Kołomański · T. Mrozek

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Section: Resultssupporting

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Coronal Mass Ejections Associated with Slow Long Duration Flares

2013

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“…One factor is the filament and its material drainage. As the evidence for this, if filament-associated CME events are excluded, the relation between the CME speed and the flare intensity is significantly increased (Chen and Zong, 2009). Another major factor might be the restraining force of the background field overlying the CME, as proposed by Török and Kliem (2007), who found that a steep decay of the background field with height leads to a fast CME and a gentle decay leads to a slow CME.…”

Section: Should Fast and Slow Cmes Be Attributed To Different Models?mentioning

confidence: 85%

Coronal Mass Ejections: Models and Their Observational Basis

Chen

2011

Living Rev. Solar Phys.

692

530

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Coronal mass ejections (CMEs) are the largest-scale eruptive phenomenon in the solar system, expanding from active region-sized nonpotential magnetic structure to a much larger size. The bulk of plasma with a mass of ∼ 10 11 -10 13 kg is hauled up all the way out to the interplanetary space with a typical velocity of several hundred or even more than 1000 km s -1 , with a chance to impact our Earth, resulting in hazardous space weather conditions. They involve many other much smaller-sized solar eruptive phenomena, such as X-ray sigmoids, filament/prominence eruptions, solar flares, plasma heating and radiation, particle acceleration, EIT waves, EUV dimmings, Moreton waves, solar radio bursts, and so on. It is believed that, by shedding the accumulating magnetic energy and helicity, they complete the last link in the chain of the cycling of the solar magnetic field. In this review, I try to explicate our understanding on each stage of the fantastic phenomenon, including their pre-eruption structure, their triggering mechanisms and the precursors indicating the initiation process, their acceleration and propagation. Particular attention is paid to clarify some hot debates, e.g., whether magnetic reconnection is necessary for the eruption, whether there are two types of CMEs, how the CME frontal loop is formed, and whether halo CMEs are special.

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“…It can be seen that there is a linear correlation between them, with the corresponding linear correlation coefficient 0.66, which is above the 95% level of confidence. However, the plot of these data also displays considerable scatter (see the discussion by Chen & Zong 2009). Both CMEs and flares may be produced by quite different mechanisms (Feynman & Hundhausen 1994) or the same mechanism but two different components of explosive magnetic-energy release (Jain et al 2010).…”

Section: Parameterizing Solar Sarsmentioning

confidence: 99%

Statistical properties of superactive regions during solar cycles 19–23

Chen

Wang

et al. 2011

A&A

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Context. Each solar activity cycle is characterized by a small number of superactive regions (SARs) that produce the most violent of space weather events with the greatest disastrous influence on our living environment. Aims. We aim to re-parameterize the SARs and study the latitudinal and longitudinal distributions of SARs. Methods. We select 45 SARs in solar cycles 21-23, according to the following four parameters: 1) the maximum area of sunspot group, 2) the soft X-ray flare index, 3) the 10.7 cm radio peak flux, and 4) the variation in the total solar irradiance. Another 120 SARs given by previous studies of solar cycles 19-23 are also included. The latitudinal and longitudinal distributions of the 165 SARs in both the Carrington frame and the dynamic reference frame during solar cycles 19-23 are studied statistically. Results. Our results indicate that these 45 SARs produced 44% of all the X class X-ray flares during solar cycles 21-23, and that all the SARs are likely to produce a very fast CME. The latitudinal distributions of SARs display the Maunder butterfly diagrams and SARs occur preferentially in the maximum period of each solar cycle. Northern hemisphere SARs dominated in solar cycles 19 and 20 and southern hemisphere SARs dominated in solar cycles 21 and 22. In solar cycle 23, however, SARs occurred about equally in each hemisphere. There are two active longitudes in both the northern and southern hemispheres, about 160• -200• apart. Applying the improved dynamic reference frame to SARs, we find that SARs rotate faster than the Carrington rate and there is no significant difference between the two hemispheres. The synodic periods are 27.19 days and 27.25 days for the northern and southern hemispheres, respectively. The longitudinal distribution of SARs is significantly non-axisymmetric and about 75% SARs occurred near two active longitudes with half widths of 45• .

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Relationship between CME velocities and X-ray fluxes of associated flares

Cited by 16 publications

References 16 publications

Coronal Mass Ejections Associated with Slow Long Duration Flares

Coronal Mass Ejections Associated with Slow Long Duration Flares

Coronal Mass Ejections: Models and Their Observational Basis

Statistical properties of superactive regions during solar cycles 19–23

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