Radio Imaging of Shock-Accelerated Electrons Associated With an Erupting Plasmoid on 2010 November 3

Bain, H. M.; Krucker, S.; Glesener, Lindsay; Lin, R. P.

doi:10.1088/0004-637x/750/1/44

Cited by 57 publications

(63 citation statements)

References 34 publications

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“…2 present a similar scenario to what was found by previous authors (Cheng et al 2011;Bain et al 2012) who were studying the behaviour just in the different SDO/AIA channels, as well as the DEM analysis from Cheng et al (2012). Given the inherent difficulties in recovering DEMs, this is reassuring that their bulk features are consistent with the original SDO/AIA data.…”

Section: Dem From Individual Pixelssupporting

confidence: 85%

“…One particular event, which peaked in GOES SXRs at 12:20 UT 2010-Nov-03 ( Fig. 1), an occulted flare and erupting plasmoid, unambiguously shows the formation of a flux rope and has subsequently been studied in detail (Reeves & Golub 2011;Cheng et al 2011;Foullon et al 2011;Bain et al 2012;Savage et al 2012;Cheng et al 2012). It is studied further in this paper.…”

Section: Introductionmentioning

confidence: 90%

“…The propagation of a metric Type II radio burst ahead of the CME in EUV is faster still (nearing 2000 km s −1 ), suggesting a piston-drive shock, in which it is moving too quickly for the ambient plasma to flow behind the driver (Bain et al 2012). This work also found that HXR emission observed with RHESSI had two non-thermal (18-40 keV) sources, one compact low in the corona, the other extended and high in the corona and close to the erupting plasmoid.…”

Section: Introductionmentioning

confidence: 99%

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Multi-thermal dynamics and energetics of a coronal mass ejection in the low solar atmosphere

Hannah

Kontar

2013

A&A

101

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Aims. The aim of this work is to determine the multi-thermal characteristics and plasma energetics of an eruptive plasmoid and occulted flare observed by the Solar Dynamics Observatory's Atmospheric Imaging Assembly (SDO/AIA). Methods. We study a 2010 Nov. 3 event (peaking at 12:20 UT in GOES soft X-rays) of a coronal mass ejection and occulted flare that demonstrates the morphology of a classic erupting flux rope. The high spatial and time resolution and six coronal channels of the SDO/AIA images allows the dynamics of the multi-thermal emission during the initial phases of eruption to be studied in detail. The differential emission measure is calculated, using an optimized version of a regularized inversion method, for each pixel across the six channels at different times, resulting in emission measure maps and movies in a variety of temperature ranges. Results. We find that the core of the erupting plasmoid is hot (8-11, 11-14 MK) with a similarly hot filamentary "stem" structure connecting it to the lower atmosphere, which could be interpreted as the current sheet in the flux rope model, though is wider than these models suggest. The velocity of the leading edge of the eruption is 597-664 km s −1 in the temperature range ≥3-4 MK and between 1029-1246 km s −1 for ≤2-3 MK. We estimate the density (in 11-14 MK) of the erupting core and stem during the impulsive phase to be about 3 × 10 9 cm −3 , 6 × 10 9 cm −3 , 9 × 10 8 cm −3 in the plasmoid core, stem, and surrounding envelope of material. This gives thermal energy estimates of 5 × 10 29 erg, 1 × 10 29 erg, and 2 × 10 30 erg. The kinetic energy for the core and envelope is slightly lower. The thermal energy of the core and current sheet grows during the eruption, suggesting continuous influx of energy presumably via reconnection. Conclusions. The combination of the optimized regularized inversion method and SDO/AIA data allows the multi-thermal characteristics (i.e. velocity, density, and thermal energies) of the plasmoid eruption to be determined.

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Section: Dem From Individual Pixelssupporting

confidence: 85%

Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

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Multi-thermal dynamics and energetics of a coronal mass ejection in the low solar atmosphere

Hannah

Kontar

2013

A&A

101

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“…8a). This event was observed by both SDO/AIA in several passbands and RHESSI simultaneously (see also Reeves and Golub 2011;Cheng et al 2011;Bain et al 2012;Glesener et al 2013), and a bright and elongated linear feature, as marked in Fig. 5c of Savage et al (2012b), that was referred to as the candidate CS was recognized within the first few minutes of the eruption.…”

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 84%

Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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We introduce how the catastrophe model for solar eruptions predicted the formation and development of the long current sheet (CS) and how the observations were used to recognize the CS at the place where the CS is presumably located. Then, we discuss the direct measurement of the CS region thickness by studying the brightness distribution of the CS region at different wavelengths. The thickness ranges from 10 4 km to about 10 5 km at heights between 0.27 and 1.16 R from the solar surface. But the traditional theory indicates that the CS is as thin as the proton Larmor radius, which is of order tens of meters in the corona. We look into the huge difference in the thickness between observations and theoretical expectations. The possible impacts that affect measurements and results are studied, and physical causes leading to a thick CS region in which reconnection can still occur at a reasonably fast rate are analyzed. Studies in both theories and observations suggest that the difference between the true value and the apparent value of the CS thickness is not significant as long as the CS could be recognised in observations. We review observations that show complex structures and flows inside the CS region and present recent numerical modelling results on some aspects of these structures. Both observations and numerical experiments indicate that the downward reconnection outflows are usually slower than the upward ones in the same eruptive event. Numerical simulations show that the complex structure inside CS and its temporal behavior as a result of turbulence and the Petschek-type slow-mode shock could probably account for the thick CS and fast reconnection. But whether the CS itself is that thick still remains unknown since, for the time being, we cannot measure the electric current directly in that region. We also review the most recent laboratory experiments of reconnection driven by energetic laser beams, and discuss some important topics for future works.

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“…The event occurred between 12:10:09 and 13:09:57 UT on the 3 November 2010 and has previously been studied in the context of the coronal mass ejection (CME) (Reeves & Golub 2011;Cheng et al 2011;Bain et al 2012), Kelvin-Helmholtz instability on the flank of the CME (Foullon et al 2011), and transverse coronal loop oscillations (White & Verwichte 2012). During this event, a CME associated with a C4.9 class flare observed by the Geostationary Operational Environmental Satellite (GOES), peaking at 12:21 UT, was observed.…”

Section: Event Overviewmentioning

confidence: 99%

First observation of a transverse vertical oscillation during the formation of a hot post-flare loop

White

Verwichte

Foullon

2012

A&A

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Aims. We report and analyse the first observation of a transverse oscillation in a hot coronal loop with the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO), following a linked coronal-flare mass-ejection event on the 3 November 2010. The oscillating coronal loop is observed off the east solar limb and exclusively in the 131 Å and 94 Å bandpasses, indicating a loop plasma of temperature in the range of 9-11 MK. Furthermore, the loop is not observed to cool into the other AIA channels, but just disappears from all bandpasses at the end of the oscillation. Methods. A time series analysis of the loop oscillation is conducted by taking several cuts at different positions along the loop, estimating the transverse displacements over time for two strands in the loop and fitting those with a damped cosine curve. Intensity time variations, both along the loop and for a series of cut cross-sections, are investigated. Using a three-dimensional loop geometry obtained from a comparison of STEREO-B/EUVI and AIA images, we model different modes of transverse oscillations in the uniformly filled loop. Results. Our time series analysis reveals a period of 302 ± 14 s (291 ± 9 s) and a damping time of 306 ± 43 s (487 ± 125 s) for the first (second) loop strand. A spatial phase shift along the loop of approximately 180 • suggests that we observe a higher order harmonic. Intensity oscillations are consistent with an interpretation in terms of a vertically polarised mode. Our forward modelling suggests that the loop oscillates as either a second or third order harmonic of this mode. Conclusions. This is the first observation of a transverse loop oscillation observed exclusively in the hot coronal lines. The loop oscillation is vertically polarised and is dominated by a higher order harmonic mode. We conclude that the excitation mechanism of this 5 min period oscillation is directly connected with the reconnection processes that form the post flare loop, which differs from the blast wave excitation mechanism often proposed as the cause of cooler transverse loop oscillations.

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Radio Imaging of Shock-Accelerated Electrons Associated With an Erupting Plasmoid on 2010 November 3

Cited by 57 publications

References 34 publications

Multi-thermal dynamics and energetics of a coronal mass ejection in the low solar atmosphere

Multi-thermal dynamics and energetics of a coronal mass ejection in the low solar atmosphere

Review on Current Sheets in CME Development: Theories and Observations

First observation of a transverse vertical oscillation during the formation of a hot post-flare loop

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