OBSERVATIONS FROMSDO,HINODE, ANDSTEREOOF A TWISTING AND WRITHING START TO A SOLAR-FILAMENT-ERUPTION CASCADE

Sterling, Alphonse C.; Moore, Ronald L.; Hara, Hirohisa

doi:10.1088/0004-637x/761/1/69

Cited by 14 publications

(10 citation statements)

References 88 publications

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“…After F6, there is a continuous slow-rise in the prominence/filament trajectory for about 6-7 hours followed by a fast-rise (after F7), for 3 hours, as observed in the SDO and STEREO images. Similar behavior of filament transition from slow-rise to fast-rise has also been studied by e.g., Sterling & Moore (2005) and Sterling et al (2012). In the present study, the slow-rise and fast-rise are apparently triggered by the flare eruptions from the active region.…”

Section: Prominence Eruptionsupporting

confidence: 88%

Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a Cme

Panesar

Sterling

Innes

et al. 2015

ApJ

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Homologous flares are flares that occur repetitively in the same active region, with similar structure and morphology. A series of at least eight homologous flares occurred in active region NOAA 11237 over 16 -17 June 2011. A nearby prominence/filament was rooted in the active region, and situated near the bottom of a coronal cavity. The active region was on the southeast solar limb as seen from SDO/AIA, and on the disk as viewed from STEREO/EUVI-B. The dual perspective allows us to study in detail behavior of the prominence/filament material entrained in the magnetic field of the repeatedly-erupting system. Each of the eruptions was mainly confined, but expelled hot material into the prominence/filament cavity system (PFCS). The field carrying and containing the ejected hot material interacted with the PFCS and caused it to inflate, resulting in a step-wise rise of the PFCS approximately in step with the homologous eruptions. The eighth eruption triggered the PFCS to move outward slowly, accompanied by a weak coronal dimming. As this slow PFCS eruption was underway, a final 'ejective' flare occurred in the core of the active region, resulting in strong dimming in the EUVI-B images and expulsion of a coronal mass ejection (CME). A plausible scenario is that the repeated homologous flares could have gradually destabilized the PFCS, and its subsequent eruption removed field above the acitive region and in turn led to the ejective flare, strong dimming, and CME.

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Section: Prominence Eruptionsupporting

confidence: 88%

Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a Cme

Panesar

Sterling

Innes

et al. 2015

ApJ

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“…It seems that first reconnection starts in the chromosphere that lead to the formation of two-ribbons, and later reconnection begins in the corona (associated with field-line rotation) resulting in the formation of a quasi-circular ribbon. The cancellation of the positive flux (P1) (before the trigger of the second C8.5 flare) may contribute to adding more flux to the newly formed flux rope to destabilize it (Sterling et al 2012). In addition, the continous shear motion between opposite polarity spots most likely aided in the buildup of magnetic energy.…”

Section: Summary and Discussionmentioning

confidence: 99%

FORMATION AND ERUPTION OF A SMALL FLUX ROPE IN THE CHROMOSPHERE OBSERVED BY NST,IRIS, ANDSDO

Kumar

Yurchyshyn

Wang

et al. 2015

ApJ

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Using high-resolution images from the 1.6 m New Solar Telescope at Big Bear Solar Observatory, we report the direct evidence of chromospheric reconnection at the polarity inversion line between two small opposite polarity sunspots. Small jetlike structures (with velocities of ∼20-55 km s ) were observed at the reconnection site before the onset of the first M1.0 flare. The slow rise of untwisting jets was followed by the onset of cool plasma inflow (∼10 km s −1 ) at the reconnection site, causing the onset of a two-ribbon flare. The reconnection between two sheared J-shaped cool Hα loops causes the formation of a small twisted (S-shaped) flux rope in the chromosphere. In addition, Helioseismic and Magnetic Imager magnetograms show the flux cancellation (both positive and negative) during the first M1.0 flare. The emergence of negative flux and the cancellation of positive flux (with shear flows) continue until the successful eruption of the flux rope. The newly formed chromospheric flux rope becomes unstable and rises slowly with a speed of ∼108 km s −1 during a second C8.5 flare that occurred after ∼3 hr of the first M1.0 flare. The flux rope was destroyed by repeated magnetic reconnection induced by its interaction with the ambient field (fan-spine topology) and looks like an untwisting surge (∼170 km s −1 ) in the coronal images recorded by the Solar Dynamics Observatory/Atmospheric Imaging Assembly. These observations suggest the formation of a chromospheric flux rope (by magnetic reconnection associated with flux cancellation) during the first M1.0 flare and its subsequent eruption/disruption during the second C8.5 flare.

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“…Some filament eruptions are followed by two ribbon flares and coronal mass ejections (CMEs), while others are not (Choudhary & Moore 2003;Chandra et al 2011). 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).…”

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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OBSERVATIONS FROMSDO,HINODE, ANDSTEREOOF A TWISTING AND WRITHING START TO A SOLAR-FILAMENT-ERUPTION CASCADE

Cited by 14 publications

References 88 publications

Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a Cme

Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a Cme

FORMATION AND ERUPTION OF A SMALL FLUX ROPE IN THE CHROMOSPHERE OBSERVED BY NST,IRIS, ANDSDO

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

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