Tracking the Evolution of a Coherent Magnetic Flux Rope Continuously From the Inner to the Outer Corona

Cheng, X.; Ding, M. D.; Guo, Yang; Zhang, J.; Vourlidas, A.; Liu, Ying D.; Olmedo, Oscar; Sun, J. Q.; Li, C.

doi:10.1088/0004-637x/780/1/28

Cited by 82 publications

(82 citation statements)

References 94 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The front of the OCBF developed speeds of up to 1200 km/s, with similar speeds for the emission peak and back positions. The average front speed of ∼800 km/s is very close to the values reported in Cheng et al (2014), while the overall average acceleration is close to 0.0 m/s 2 . The thickness of the wave increased for most of the period, before decreasing towards the end.…”

Section: June 7 2011 Eventsupporting

confidence: 81%

The Coronal Analysis of SHocks and Waves (CASHeW) framework

Kozarev

Davey

Kendrick

et al. 2017

J. Space Weather Space Clim.

View full text Add to dashboard Cite

-Coronal bright fronts (CBF) are large-scale wavelike disturbances in the solar corona, related to solar eruptions. They are observed (mostly in extreme ultraviolet (EUV) light) as transient bright fronts of finite width, propagating away from the eruption source location. Recent studies of individual solar eruptive events have used EUVobservations of CBFs and metric radio type II burst observations to show the intimate connection between waves in the low corona and coronal mass ejection (CME)-driven shocks. EUV imaging with the atmospheric imaging assembly instrument on the solar dynamics observatory has proven particularly useful for detecting large-scale short-lived CBFs, which, combined with radio and in situ observations, holds great promise for early CME-driven shock characterization capability. This characterization can further be automated, and related to models of particle acceleration to produce estimates of particle fluxes in the corona and in the near Earth environment early in events. We present a framework for the coronal analysis of shocks and waves (CASHeW). It combines analysis of NASA Heliophysics System Observatory data products and relevant data-driven models, into an automated system for the characterization of off-limb coronal waves and shocks and the evaluation of their capability to accelerate solar energetic particles (SEPs). The system utilizes EUV observations and models written in the interactive data language. In addition, it leverages analysis tools from the SolarSoft package of libraries, as well as third party libraries. We have tested the CASHeW framework on a representative list of coronal bright front events. Here we present its features, as well as initial results. With this framework, we hope to contribute to the overall understanding of coronal shock waves, their importance for energetic particle acceleration, as well as to the better ability to forecast SEP events fluxes.

show abstract

Section: June 7 2011 Eventsupporting

confidence: 81%

The Coronal Analysis of SHocks and Waves (CASHeW) framework

Kozarev

Davey

Kendrick

et al. 2017

J. Space Weather Space Clim.

View full text Add to dashboard Cite

show abstract

“…Therefore, it is also possible that the initial structure above the filament is a part of the flux rope observed later during magnetic reconnection. The observed structure (after 07:10 UT) most likely is a magnetic flux rope because (i) it is observed only in the AIA hot channels (AIA 131 and 94 Å), whose morphology and temperature (T ∼ 8 MK) are quite similar to the flux ropes reported in recent case studies Patsourakos et al 2013;Cheng et al 2014). (ii) The structure is aligned and appeared above the neutral line (along the flare ribbons observed in the AIA 1600 Å) and the orientation of the structure is across the post flare arcade (cusp) loops formed after the eruption (see Fig.…”

Section: Flux Rope Formation and Eruptionsupporting

confidence: 64%

“…The flux rope expanded slowly and developed into a large-scale structure possibly by magnetic reconnection with the surrounding magnetic fields within 15−20 min. Cheng et al (2014) also reported a similar flux rope structure with twisted or helical threads in hot AIA channels for a different eruptive event. Li & Zhang (2013) studied the four homologous flux rope structures that appeared during the magnetic reconnection in AIA hot channels.…”

Section: Summary and Discussionmentioning

confidence: 62%

“…In addition, a twisted flux rope structure is sometime observed co-spatially in soft X-ray and extreme ultraviolet (EUV) channels (hot and cool channels) above the neutral line (Kumar et al 2011b). Recently, flux ropes have been observed in the AIA hot channels (131 and 94 Å, T ∼ 8 MK), which are elongated Sshaped structures Patsourakos et al 2013;Cheng et al 2014). Expansion and rise of these structures are associated with the formation of CMEs in the low corona.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Multiwavelength observation of a large-scale flux rope eruption above a kinked small filament

Kumar

Cho

2014

A&A

View full text Add to dashboard Cite

We analyzed multiwavelength observations of a western limb flare (C3.9) that occurred in AR NOAA 111465 on 30 April 2012. The high-resolution images recorded by SDO/AIA 304, 1600 Å and Hinode/SOT Hα show the activation of a small filament (rising speed ∼ 40 km s −1 ) associated with a kink instability and the onset of a C-class flare near the southern leg of the filament. The first magnetic reconnection occurred at one of the footpoints of the filament and caused the breaking of its southern leg. The filament shows unwinding motion of the northern leg and apex in counterclockwise direction and failed to erupt. A flux-rope structure (visible only in hot channels, i.e., AIA 131 and 94 Å and Hinode/SXT) appeared along the neutral line during the second magnetic reconnection that occurred above the kinked filament. The formation of the RHESSI hard X-ray source (12−25 keV) above the kinked filament and the simultaneous appearance of the hot 131 Å loops associated with photospheric brightenings (AIA 1700 Å) indicates the particle acceleration along these loops from the top of the filament. In addition, extreme ultraviolet disturbances or waves observed above the filament in 171 Å also show a close association with magnetic reconnection. The flux rope rises slowly (∼100 km s −1 ), which produces a very large twisted structure possibly through reconnection with the surrounding sheared magnetic fields within ∼15−20 min, and showed an impulsive acceleration reaching a height of about 80-100 Mm. AIA 171 and SWAP 174 Å images reveal a cool compression front (or coronal mass ejection frontal loop) surrounding the hot flux rope structure.

show abstract

“…Gopalswamy et al (2014) estimated that the peak speed of the CME was ∼1880 km s −1 . The early kinematics of the primary CME has been studied by Cheng et al (2014). They found that the magnetic flux rope, i.e., the primary CME, started to accelerate around 12:31 UT.…”

Section: The 2013 May 22 Solar Eruptionsmentioning

confidence: 99%

Source Regions of the Type Ii Radio Burst Observed During a Cme–cme Interaction on 2013 May 22

Mäkelä

Gopalswamy

Reiner

et al. 2016

ApJ

View full text Add to dashboard Cite

We report on our study of radio source regions during the type II radio burst on 2013 May 22 based on directionfinding analysis of the Wind/WAVES and STEREO/WAVES (SWAVES) radio observations at decameterhectometric wavelengths. The type II emission showed an enhancement that coincided with the interaction of two coronal mass ejections (CMEs) launched in sequence along closely spaced trajectories. The triangulation of the SWAVES source directions posited the ecliptic projections of the radio sources near the line connecting the Sun and the STEREO-A spacecraft. The WAVES and SWAVES source directions revealed shifts in the latitude of the radio source, indicating that the spatial location of the dominant source of the type II emission varies during the CME-CME interaction. The WAVES source directions close to 1 MHz frequencies matched the location of the leading edge of the primary CME seen in the images of the LASCO/C3 coronagraph. This correspondence of spatial locations at both wavelengths confirms that the CME-CME interaction region is the source of the type II enhancement. Comparison of radio and white-light observations also showed that at lower frequencies scattering significantly affects radio wave propagation.

show abstract

Tracking the Evolution of a Coherent Magnetic Flux Rope Continuously From the Inner to the Outer Corona

Cited by 82 publications

References 94 publications

The Coronal Analysis of SHocks and Waves (CASHeW) framework

The Coronal Analysis of SHocks and Waves (CASHeW) framework

Multiwavelength observation of a large-scale flux rope eruption above a kinked small filament

Source Regions of the Type Ii Radio Burst Observed During a Cme–cme Interaction on 2013 May 22

Contact Info

Product

Resources

About