Multiwavelength Observations of a Failed Flux Rope in the Eruption and Associated M-Class Flare from NOAA AR 11045

Kumar, Pankaj; Srivastava, A. K.; Filippov, B. P.; Erdélyi, R.; Uddin, Wahab

doi:10.1007/s11207-011-9829-z

Cited by 29 publications

(26 citation statements)

References 42 publications

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“…The stability of the flux rope depends on the strength of the total electric current flowing within it and properties of the surrounding coronal magnetic field. The change of equilibrium conditions within the flux rope may also be accompanied with the flux emergence (a classical trigger of eruption; e.g, Kumar et al 2011). There is a critical height for the stable flux-rope equilibrium in any given magnetic field.…”

Section: Discussionmentioning

confidence: 99%

Solar Magnetic Flux Ropes

et al. 2015

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The most probable initial magnetic configuration of a CME is a flux rope consisting of twisted field lines which fill the whole volume of a dark coronal cavity. The flux ropes can be in stable equilibrium in the coronal magnetic field for weeks and even months, but suddenly they loose their stability and erupt with high speed. Their transition to the unstable phase depends on the parameters of the flux rope (i.e., total electric current, twist, mass loading etc.), as well as on the properties of the ambient coronal magnetic field. One of the major governing factors is the vertical gradient of the coronal magnetic field which is estimated as decay index (n). Cold dense prominence material can be collected in the lower parts of the helical flux tubes. Filaments are therefore good tracers of the flux ropes in the corona, which become visible long before the beginning of the eruption. The perspectives of the filament eruptions and following CMEs can be estimated by the comparison of observed filament heights with calculated decay index distributions. The present paper reviews the formation of magnetic flux ropes, their stable and unstable phases, eruption conditions, and also discusses their physical implications in the solar corona.Comment: 27 pages, 14 figures; to appear in Journal of Astrophysics & Astronomy (Special Issue; Eds: V. Fedun, A.K. Srivastava, R. Erdelyi, J.C. Pandey

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Section: Discussionmentioning

confidence: 99%

Solar Magnetic Flux Ropes

et al. 2015

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“…Using the STEREO/EUVI 304 Å movies 1 and 195 Å movies of AR 11045, we found 29 filament eruptions 1 , and 19 EUV waves 1 during the AR active phase. Table 1 lists the information of 8 M-class flares and their associated 5 CMEs and 3 filament eruptions, of which the event on February 12 has been studied by Kumar et al (2011). Columns 1-6 in Table 1 show the date, the beginning time, the peak time, the ending time, the class and the heliographic position of the flares, and Cols.…”

Section: Flares Cmes Filament Eruptions and Euv Waves In Ar 11045mentioning

confidence: 99%

Study of the first productive active region in solar cycle 24

Zhang

et al. 2012

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Context. The Sun is very quiet with less sunspots and activity since the beginning of solar cycle 24. However, the active region (AR) 11 045 emerged on February 5, 2010, is associated with 43 (8 M-and 35 C-class) flares, 53 coronal mass ejections (CMEs), 29 filament eruptions, 19 extreme ultraviolet (EUV) waves and abundant jets, indicating that this AR is the first productive one of solar cycle 24. Aims. We study the AR evolution and its associated activities, and also their relationships, to understand this productive AR. Methods. We used SOHO/MDI magnetograms to study the magnetic fields, STEREO/SECCHI images to explore the activities, and GOES measurements to investigate the soft X-ray flux of the AR. Results. During the AR evolution, six pairs of main magnetic fields emerged, and 93.1% flares and 82.75% filament eruption occurred in the emergence and stable phases of the magnetic flux. However, 43.4% CMEs occurred in the decaying phase, even though there were less flares. An example is given to show that an event is related to a flare, a filament eruption, a CME and an EUV wave from inner corona to outer corona in space, and the filament eruption and EUV wave occur near the peak time of the flare. Among the 29 filament eruptions, 79.3% are associated with CMEs, as well as 58.6%, associated with flares, and 34.5%, associated with EUV waves. During the 12-day active phase, 575 jets are detected with a daily occurrence rate of 49.3. This is the first time that so many jets have been identified in one AR, implying at least 575 lower magnetic reconnection processes during the AR evolution. We statistically studied these jets along with the AR evolution, and noticed that the jets mostly occurred surrounding the emerging flux. We also investigated the spatio-temporal relationships between the jets and the flares, and find that the jets are usually rooted around the flare cores, and the soft X-ray flux is inverse correlated with the number of the jets, especially during the beginning 9 days since the AR emergence. In comparison with AR 11045, we studied the other newly emerging AR 11045, and obtained similar results. The relationships between the jets and the flares may well represent a scenario of two-step magnetic reconnection. Using schematic diagrams, we explain the remarkable magnetic field emergence, cancelation and shear motion of AR 11045, and its associated activities.

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“…During a full eruption, all of the magnetic field and plasma eject out into the interplanetary space in the form of a CME (Sterling et al 2012;Chandra et al 2010;Joshi et al 2013b). In the case of failed eruption, however, material and the magnetic field remain confined in the corona (Ji et al 2003;Török & Kliem 2005;Liu et al 2009;Kumar et al 2011;Joshi et al 2013a;Kuridze et al 2013). Partial filament eruption is characterized as an eruption during which some of the material erupts while some of it stays in equilibrium or falls back onto the Sun (Tripathi et al 2009;Shen et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Confined Partial Filament Eruption and Its Reformation Within a Stable Magnetic Flux Rope

Joshi

Srivastava

Filippov

et al. 2014

ApJ

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We present observations of a confined partial eruption of a filament on 2012 August 4, which restores its initial shape within ≈2 hr after eruption. From the Global Oscillation Network Group Hα observations, we find that the filament plasma turns into dynamic motion at around 11:20 UT from the middle part of the filament toward the northwest direction with an average speed of ≈105 km s −1. A little brightening underneath the filament possibly shows the signature of low-altitude reconnection below the filament eruptive part. In Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å images, we observe an activation of right-handed helically twisted magnetic flux rope that contains the filament material and confines it during its dynamical motion. The motion of cool filament plasma stops after traveling a distance of ≈215 Mm toward the northwest from the point of eruption. The plasma moves partly toward the right foot point of the flux rope, while most of the plasma returns after 12:20 UT toward the left foot point with an average speed of ≈60 km s −1 to reform the filament within the same stable magnetic structure. On the basis of the filament internal fine structure and its position relative to the photospheric magnetic fields, we find filament chirality to be sinistral, while the activated enveloping flux rope shows a clear right-handed twist. Thus, this dynamic event is an apparent example of one-to-one correspondence between the filament chirality (sinistral) and the enveloping flux rope helicity (positive). From the coronal magnetic field decay index, n, calculation near the flux rope axis, it is evident that the whole filament axis lies within the domain of stability (i.e., n < 1), which provides the filament stability despite strong disturbances at its eastern foot point.

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Multiwavelength Observations of a Failed Flux Rope in the Eruption and Associated M-Class Flare from NOAA AR 11045

Cited by 29 publications

References 42 publications

Solar Magnetic Flux Ropes

Solar Magnetic Flux Ropes

Study of the first productive active region in solar cycle 24

Confined Partial Filament Eruption and Its Reformation Within a Stable Magnetic Flux Rope

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