A Model for Magnetically Coupled Sympathetic Eruptions

Török, Tibor; Panasenco, O.; Titov, V. S.; Mikić, Z.; Reeves, Katharine K.; Velli, Marco; Linker, J. A.; Toma, G. de

doi:10.1088/2041-8205/739/2/l63

Cited by 193 publications

(238 citation statements)

References 46 publications

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“…Quite possibly, this destabilization makes the adjoining west part of the AR to reconfigure its magnetic field (similar to e.g. Török et al 2011), eventually triggering there an X1.3 flare there and the CME on March 7, 01:05 UT. The propagation of the CMEs in the interplanetary medium and its effects on Earth were studied by Patsourakos et al (2016).…”

Section: Discussionmentioning

confidence: 99%

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The spectroscopic imprint of the pre-eruptive configuration resulting into two major coronal mass ejections

Syntelis

Gontikakis

Patsourakos

et al. 2016

A&A

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Aims. We present a spectroscopic analysis of the pre-eruptive configuration of active region NOAA 11429, prior to two very fast coronal mass ejections (CMEs) on March 7, 2012 that are associated with this active region. We study the thermal components and the dynamics associated with the ejected flux ropes. Methods. Using differential emission measure (DEM) analysis of Hinode/EIS and SDO/AIA observations, we identify the emission components of both the flux rope and the host active region. We then follow the time evolution of the flux rope emission components by using AIA observations. The plasma density and the Doppler and non-thermal velocities associated with the flux ropes are also calculated from the EIS data. Results. The eastern and western parts of the active region, in which the two different fast CMEs originated during two X-class flares, were studied separately. In both regions we identified an emission component in the temperature range of log T = 6.8−7.1 associated with the presence of flux ropes. The time evolution of the eastern region showed an increase in the mean DEM in this temperature range by an order of magnitude, 5 h prior to the first CME. This was associated with a gradual rise and heating of the flux rope as manifested by blue-shifts and increased non-thermal velocities in Ca xv 200.97 Å, respectively. An overall upward motion of the flux ropes was measured (relative blue-shifts of ∼12 km s −1 ). The measured electron density was found to be 4 × 10 9 −2 × 10 10 cm −3 (using the ratio of Ca xv 181.90 Å over Ca xv 200.97 Å). We compare our findings with other works on the same AR to provide a unified picture of its evolution.

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Section: Discussionmentioning

confidence: 99%

“…Kusano et al 2004), flux emergence (e.g. Chen & Shibata 2000), sympathetic eruptions (Török et al 2011), combinations of the above, etc. Energy release and plasma heating is expected during both the formation and the destabilization of a FR.…”

Section: Introductionmentioning

confidence: 99%

The spectroscopic imprint of the pre-eruptive configuration resulting into two major coronal mass ejections

Syntelis

Gontikakis

Patsourakos

et al. 2016

A&A

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“…On the other hand consecutive eruptions either in a single AR or in different regions, (commonly called sympathetic eruptions) reveal global connection of the magnetic field and give us an important clue to the eruption process (Schrijver & Title 2011). The details of how one eruption can trigger another one at a significant distance are well demonstrated in the MHD simulations by Török et al (2011). By adopting a similar mechanism, it can be explained how the development of the observed QCSR during Flare II may have been initiated by Flare I sigmoid eruption.…”

Section: Quasi-circular Secondary Ribbonmentioning

confidence: 92%

Observation of a Large-scale Quasi-circular Secondary Ribbon Associated with Successive Flares and a Halo CME

Lim

Yurchyshyn

Kumar

et al. 2017

ApJ

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Solar flare ribbons provide an important clue to the magnetic reconnection process and associated magnetic field topology in the solar corona. We detected a large-scale secondary flare ribbon of a circular shape that developed in association with two successive M-class flares and one CME. The ribbon revealed interesting properties such as 1) a quasi-circular shape and enclosing the central active region; 2) the size as large as 500 by 650 , 3) successive brightenings in the clockwise direction at a speed of 160 km sstarting from the nearest position to the flaring sunspots, 4) radial contraction and expansion in the northern and the southern part, respectively at speeds of ≤ 10 km s −1. Using multi-wavelength data from SDO, RHESSI, XRT, and Nobeyama, along with magnetic field extrapolations, we found that: 1) the secondary ribbon location is consistent with the field line footpoints of a fan-shaped magnetic structure that connects the flaring region and the ambient decaying field; 2) the second M2.6 flare occurred when the expanding coronal loops driven by the first M2.0 flare encountered the background decayed field. 3) Immediately after the second flare, the secondary ribbon developed along with dimming regions. Based on our findings, we suggest that interaction between the expanding sigmoid field and the overlying fan-shaped field triggered the secondary reconnection that resulted in the field opening and formation of the quasi-circular secondary ribbon. We thus conclude that interaction between the active region and the ambient large-scale fields should be taken into account to fully understand the entire eruption process.

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“…The interaction of two nearby filament channels with different filament chiralities within a large-scale coronal fanspine magnetic structure have not been observed before, although fan-spine configurations have been discussed in the case of solar eruptions in "pseudostreamers" (Wang et al 2007;Török et al 2011b;Rachmeler et al 2014;Yang et al 2015), jets (Filippov et al 2009(Filippov et al , 2015Pariat et al 2009), and flares Joshi et al 2015).…”

Section: The Observations As Well As the Pfss Calculations Clearlymentioning

confidence: 99%

Interaction of Two Filament Channels of Different Chiralities

Joshi

Filippov

Schmieder

et al. 2016

ApJ

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We present observations of the interactions between the two filament channels of different chiralities and associated dynamics that occurred during 2014 April 18-20. While two flux ropes of different helicity with parallel axial magnetic fields can only undergo a bounce interaction when they are brought together, the observations at first glance show that the heated plasma is moving from one filament channel to the other. The SDO/AIA 171 Å observations and the potential-field source-surface magnetic field extrapolation reveal the presence of a fan-spine magnetic configuration over the filament channels with a null point located above them. Three different events of filament activations, partial eruptions, and associated filament channel interactions have been observed. The activation initiated in one filament channel seems to propagate along the neighboring filament channel. We believe that the activation and partial eruption of the filaments brings the field lines of flux ropes containing them closer to the null point and triggers the magnetic reconnection between them and the fan-spine magnetic configuration. As a result, the hot plasma moves along the outer spine line toward the remote point. Utilizing the present observations, for the first time we have discussed how two different-chirality filament channels can interact and show interrelation.

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A Model for Magnetically Coupled Sympathetic Eruptions

Cited by 193 publications

References 46 publications

The spectroscopic imprint of the pre-eruptive configuration resulting into two major coronal mass ejections

The spectroscopic imprint of the pre-eruptive configuration resulting into two major coronal mass ejections

Observation of a Large-scale Quasi-circular Secondary Ribbon Associated with Successive Flares and a Halo CME

Interaction of Two Filament Channels of Different Chiralities

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