A Quadruple Magnetic Source Model for Arcade Flares and X‐Ray Arcade Formations outside Active Regions. II. Dark Filament Eruption and the Associated Arcade Flare

Hirose, Shigenobu; Uchida, Yutaka; Uemura, Shun; Yamaguchi, Takuma; Cable, S.

doi:10.1086/320084

Cited by 50 publications

(32 citation statements)

References 33 publications

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“…In the 2D quadrupolar flare model (Hirose et al 2001) the initial configuration consists of two parallel arcades and three parallel neutral lines. The driver is a converging flow pattern that pushes the two arcades together.…”

Section: Scientific Models For Solar Flaresmentioning

confidence: 99%

Solar Weather Event Modelling and Prediction

et al. 2009

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Key drivers of solar weather and mid-term solar weather are reviewed by considering a selection of relevant physics-and statistics-based scientific models as well as a selection of related prediction models, in order to provide an updated operational scenario for space weather applications. The characteristics and outcomes of the considered scientific and prediction models indicate that they only partially cope with the complex nature of solar activity for the lack of a detailed knowledge of the underlying physics. This is indicated by the fact that, on one hand, scientific models based on chaos theory and non-linear dynamics reproduce better the observed features, and, on the other hand, that prediction models based on statistics and artificial neural networks perform better. To date, the solar weather prediction success at most time and spatial scales is far from being satisfactory, but the forthcoming ground-and space-based high-resolution observations can add fundamental tiles to the modelling and predicting frameworks as well as the application of advanced mathematical approaches in the analysis of diachronic solar observations, that are a must to provide comprehensive and homogeneous data sets.

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Section: Scientific Models For Solar Flaresmentioning

confidence: 99%

Solar Weather Event Modelling and Prediction

et al. 2009

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“…More specifically, the magnetic field can become stressed (i.e., non-potential) and therefore can increase its energy when shearing, converging or twisting motions of the footpoints of its field lines take place (Priest et al 1994;Hirose et al 2001;Antiochos et al 1999). In addition, an unstable Now at Max-Planck-Institut für Sonnensystemforschung.…”

Section: Introductionmentioning

confidence: 99%

The role of filament activation in a solar eruption

Costa

Zuccarello

Fletcher

et al. 2012

A&A

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Context. Observations show that the mutual relationship between filament eruptions and solar flares cannot be described in terms of an unique scenario. In some cases, the eruption of a filament appears to trigger a flare, while in others the observations are more consistent with magnetic reconnection that produces both the flare observational signatures (e.g., ribbons, plasma jets, post-flare loops, etc.) and later the destabilization and eruption of a filament. Aims. Contributing to a better comprehension of the role played by filament eruptions in solar flares, we study an event which occurred in NOAA 8471, where a flare and the activation of (at least) two filaments were observed on 28 February 1999. Methods. By using imaging data acquired in the 1216, 1600, 171 and 195 Å TRACE channels and by BBSO in the continnum and in the Hα line, a morphological study of the event is carried out. Moreover, using TRACE 1216 and 1600 Å data, an estimate of the "pure" Lyα power is obtained. The extrapolation of the magnetic field lines is done using the SOHO/MDI magnetograms and assuming a potential field. Results. Initially an area hosting a filament located over a δ spot becomes brighter than the surroundings, both in the chromosphere and in the corona. This area increases in brightness and extension, eventually assuming a two-ribbon morphology, until it reaches the eastern part of the active region. Here a second filament becomes activated and the brightening propagates to the south, passing over a large supergranular cell. The potential magnetic field extrapolation indicates that the field line connectivity changes after the flare. Conclusions. The event is triggered by the destabilization of a filament located between the two polarities of a δ spot. This destabilization involves the magnetic arcades of the active region and causes the eruption of a second filament, that gives rise to a CME and to plasma motions over a supergranular cell. We conclude that in this event the two filaments play an active and decisive role, albeit in different stages of the phenomenon, in fact the destabilization of one filament causes brightenings, reconnection and ribbons, while the second one, whose eruption is caused by the field reconfiguration resulting from the previous reconnection, undergoes the greatest changes and causes the CME.

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“…We also highlight the CSHKP 2D standard model (Carmichael 1964;Sturrock 1966;Hirayama 1974;Kopp & Pneuman 1976) based on the assumption that the initial driver is a rising filament stretching a current sheet, where the Sweet-Parker or Petscheck reconnection can occur. In the twodimensional quadrupolar flare model (Hirose et al 2001), the initial configuration consists of two parallel arcades pushed toward each other by a converging flow pattern. The X-point above the middle neutral line supports a filament that becomes unstable owing to the tearing-mode instability, triggering anomalous resistivity and fast reconnection.…”

Section: Introductionmentioning

confidence: 99%

Filament destabilization and CME release during a long duration flare

Zuccarello

Contarino

Fárník

et al. 2011

A&A

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Context. During complex and long duration solar flares, several filament destabilizations or eruptions can occur that are often related to coronal mass ejections (CMEs). Aims. We describe the study of an X3.8 long duration event (LDE) that occurred in NOAA 10720 on 17 January 2005 and was characterized by three filament destabilizations and two CMEs. Methods. Using multi-wavelength data provided by both ground-based instruments and satellites, in addition to MDI magnetograms, we investigated the morphological and magnetic evolution of the active region before and during the LDE. Results. Our analysis of H α and 1600 Å images showed that initially a two-ribbon structure developed in the central part of the active region, where a filament was previously observed. At a later time, two bright ribbons (in the most eastern side) and a strong brightness increase (at the western outskirt of the active region) were simultaneously observed. In a subsequent time interval, a new pair of ribbons was observed in the western side of the active region. Moreover, a linear force-free field extrapolation helped identify a null point in the central part of the active region. Conclusions. The initial filament destabilization that occurred in the central part of NOAA 10720 was probably due to magnetic flux emergence and photospheric shearing motions, which caused a slow tether-cutting process beneath the filament. The rearrangement of the magnetic field configuration, occurring in the same area as the location of the null point, changed the magnetic field connectivity in the active region, triggering two filament eruptions in the eastern and western part of the active region and two halo CMEs, in a kind of domino effect.

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A Quadruple Magnetic Source Model for Arcade Flares and X‐Ray Arcade Formations outside Active Regions. II. Dark Filament Eruption and the Associated Arcade Flare

Cited by 50 publications

References 33 publications

Solar Weather Event Modelling and Prediction

Solar Weather Event Modelling and Prediction

The role of filament activation in a solar eruption

Filament destabilization and CME release during a long duration flare

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