Successive Flaring during the 2005 September 13 Eruption

Wang, Haimin; Liu, Chang; Jing, Ju; Yurchyshyn, Vasyl

doi:10.1086/522911

Cited by 27 publications

(25 citation statements)

References 32 publications

(38 reference statements)

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“…3, left panel), approximately 3 h prior to its eruption at ∼19:24 UT. Other studies of this filament eruption have been carried out independently by Nagashima et al (2007) and Wang et al (2007). We observed the activation of the filament mainly in TRACE images taken in the 195 Å passband (Fig.…”

Section: September 13 (Event 1: On-disk)supporting

confidence: 67%

“…Events 4 and 5 of Table 1 are two examples of such eruptions. Earlier observations reported by Wang & Shi (1993) showed a filament eruption characterised by an untwisting upward motion associated with a localised precursor "microflare" representing the first signature for the disturbance of the system. In conformity with the conclusions drawn from event 4 discussed in this paper, Wang & Shi (1993) found that canceling magnetic reconnection beneath the filament can be responsible for the untwisting and upward motion.…”

Section: Discussionmentioning

confidence: 92%

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X-ray precursors to flares and filament eruptions

Chifor¹,

Tripathi²,

Mason³

et al. 2007

A&A

103

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Aims. To study preflare X-ray brightenings as diagnostics of the destabilisation of flare-associated erupting filaments/prominences. Methods. We combine new observations from the Transition Region and Coronal Explorer (TRACE) and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), as well as revisit events reported in the literature to date, in order to scrutinise the preflare activity during eight flare-associated filament eruptions. Results. The preflare activity occurs in the form of discrete, localised X-ray brightenings observed between 2 and 50 min before the impulsive phase of the flare and filament acceleration. These transient preflare brightenings are situated on or near (within 10 of) the polarity inversion line (PIL), coincident with emerging and/or canceling magnetic flux. The filaments begin to rise from the location of the preflare brightenings. In five out of eight events, the preflare brightenings were observed beneath the filament channel, close to the filament footpoint first observed to rise. Both thermal and nonthermal hard X-ray emissions during the preflare enhancement were detected with RHESSI, suggesting that both plasma heating and electron acceleration occurred at this time. The main energy release during the impulsive phase of the flare is observed close to (within 50 of) the preflare brightenings. The fast-rise phase of the filament eruption starts at the same time as the onset of the main flare or up to 5 min later. Conclusions. The preflare brightenings are precursors to the flare and filament eruption. These precursors represent distinct, localised instances of energy release, rather than a gradual energy release prior to the main flare. The X-ray precursors represent clearly observable signatures in the early stages of the eruption. Together with the timing of the filament fast-rise at or after the main flare onset, the X-ray precursors provide evidence for a tether-cutting mechanism initially manifested as localised magnetic reconnection being a common trigger for both flare emission and filament eruption.

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Section: September 13 (Event 1: On-disk)supporting

confidence: 67%

Section: Discussionmentioning

confidence: 92%

X-ray precursors to flares and filament eruptions

Chifor¹,

Tripathi²,

Mason³

et al. 2007

A&A

103

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“…Namely, the transverse field near the magnetic polarity inversion line (PIL) at the core flaring region is enhanced rapidly and irreversibly, which is often accompanied by an increase of magnetic shear. Such a rapid change of vector PMFs closely associated with flares/CMEs has been consistently found later on using ground-based (Schmieder et al 1994;Wang et al 2002Wang et al , 2004bWang et al , 2005Wang et al , 2007Liu et al 2005;Su et al 2011) and Hinode observations (Jing et al 2008;Li et al 2009). Indirect evidence includes the unbalanced flux evolution of the line-of-sight magnetic field , the variation of the sunspot white-light structure in flaring regions (Wang et al 2004a;Deng et al 2005;Liu et al 2005;Chen et al 2007), and the change in the pattern of the penumbral Evershed flow (Deng et al 2011).…”

Section: Introductionsupporting

confidence: 58%

Rapid Changes of Photospheric Magnetic Field After Tether-Cutting Reconnection and Magnetic Implosion

Liu

Deng

et al. 2011

ApJ

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The rapid, irreversible change of the photospheric magnetic field has been recognized as an important element of the solar flare process. This Letter reports such a rapid change of magnetic fields during the 2011 February 13 M6.6 flare in NOAA AR 11158 that we found from the vector magnetograms of the Helioseismic and Magnetic Imager (HMI) with 12 minute cadence. High-resolution magnetograms of Hinode that are available at ∼−5.5, −1.5, 1.5, and 4 hr relative to the flare maximum are used to reconstruct a three-dimensional coronal magnetic field under the nonlinear force-free field (NLFFF) assumption. UV and hard X-ray images are also used to illuminate the magnetic field evolution and energy release. The rapid change is mainly detected by HMI in a compact region lying in the center of the magnetic sigmoid, where the mean horizontal field strength exhibited a significant increase of 28%. The region lies between the initial strong UV and hard X-ray sources in the chromosphere, which are cospatial with the central feet of the sigmoid according to the NLFFF model. The NLFFF model further shows that strong coronal currents are concentrated immediately above the region, and that, more intriguingly, the coronal current system underwent an apparent downward collapse after the sigmoid eruption. These results are discussed in favor of both the tether-cutting reconnection producing the flare and the ensuing implosion of the coronal field resulting from the energy release.

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“…It occurred from 23:15 to 23:30 UT on 2005 September 13 in AR 10808. Several papers analyzed this event and associated phenomena, for example, the related radio bursts (Oberoi et al 2009), or CME (Wang et al 2007;Liu et al 2009), or filament (Nagashima et al 2007), or magnetic configuration (Li et al 2007). Figure 1 shows the SOHO/MDI magnetogram at 23:23:03 UT with RHESSI (PIXON) contours at 23:18:00 UT (a) and 23:19:30 UT (b) respectively.…”

Section: Observation and Measurementmentioning

confidence: 99%

Radiative and conductive cooling in a solar flare

Ning

Liu

2011

Astrophys Space Sci

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We investigate the radiative and conductive cooling in the solar flare observed by RHESSI on 2005 September 13. The radiative and conductive loss energies are estimated from the observations after the flare onset. Consistent with previous findings, the cooling is increased with time, especially the radiation becomes remarkable on the later phase of flare. According our method, about half of thermal energy is traced by RHESSI soft X-rays, while the other half is lost by the radiative (∼38%) and conductive (∼9%) cooling at end of the hard X-rays in this event. The nonthermal energy input of P nth (inferred from RHESSI hard X-ray spectrum) is not well correlated with the derivative of thermal energy of dE th dt (required to radiate the RHESSI soft X-ray flux and spectrum) alone. However, after consideration the radiation and conduction, a high correlation is obtained between the derivative of total thermal energy ( dE th +E rad +E cond dt ) and nonthermal energy input (P nth ) from the flare start to end, indicating the relative importance of conductive and direct radiative losses during the solar flare development. Ignoring the uncertainties to estimate the energy from the observations, we find that about ∼12% fraction of the known energy is transferred into the thermal energy for the 2005 September 13 flare.

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Successive Flaring during the 2005 September 13 Eruption

Cited by 27 publications

References 32 publications

X-ray precursors to flares and filament eruptions

X-ray precursors to flares and filament eruptions

Rapid Changes of Photospheric Magnetic Field After Tether-Cutting Reconnection and Magnetic Implosion

Radiative and conductive cooling in a solar flare

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