Plasma Evolution within an Erupting Coronal Cavity

Long, David M.; Harra, L. K.; Matthews, Sarah; Warren, Harry P.; Lee, Kyoung‐Sun; Doschek, G. A.; Hara, Hirohisa; Jenkins, Jack

doi:10.3847/1538-4357/aaad68

Cited by 31 publications

(39 citation statements)

References 35 publications

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“…we made the EOVSA images at one-quarter of the available resolution of 1 s). The initial rise of the ejecta and flux rope during the first 10 minutes, which were studied by Doschek et al (2018) and Long et al (2018), manifests as an upward-moving feature apparent in the AIA 193Å and 131Å data, outlined with black-dashed curves in Fig. 3a and 3b, respectively.…”

Section: Temporal Developmentmentioning

confidence: 91%

“…The event has received considerable attention in the literature in the few months since it occurred (e.g. Warren et al 2018;Yan et al 2018;Li et al 2018;Long et al 2018;Omodei et al 2018;Doschek et al 2018). Figure 1 shows an overview of spatially-integrated lightcurves for emission at different wavelengths, and the total power microwave dynamic spectrum from EOVSA.…”

Section: Observationsmentioning

confidence: 99%

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Microwave and Hard X-Ray Observations of the 2017 September 10 Solar Limb Flare

Gary

Bin

Dennis

et al. 2018

ApJ

208

168

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We report the first science results from the newly completed Expanded Owens Valley Solar Array (EOVSA), which obtained excellent microwave imaging spectroscopy observations of SOL2017-09-10, a classic partially-occulted solar limb flare associated with an erupting flux rope. This event is also well-covered by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in hard X-rays (HXRs). We present an overview of this event focusing on microwave and HXR data, both associated with high-energy nonthermal electrons, and discuss them within the context of the flare geometry and evolution revealed by extreme ultraviolet (EUV) observations from the Atmospheric Imaging Assembly aboard the Solar Dynamics Observatory (SDO/AIA). The EOVSA and RHESSI data reveal the evolving spatial and energy distribution of high-energy electrons throughout the entire flaring region. The results suggest that the microwave and HXR sources largely arise from a common nonthermal electron population, although the microwave imaging spectroscopy provides information over a much larger volume of the corona.

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Section: Temporal Developmentmentioning

confidence: 91%

Section: Observationsmentioning

confidence: 99%

Microwave and Hard X-Ray Observations of the 2017 September 10 Solar Limb Flare

Gary

Bin

Dennis

et al. 2018

ApJ

208

168

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“…The launch of the extremely fast erupting MFR and CME likely drove a global shock ahead of it indicated by the extreme ultraviolet (EUV) waves (or EIT waves, Dere et al, ) in SUVI's 195 Å passband (Figure b and better shown in a movie in the online version of Seaton & Darnel, ). This strong EUV wave had a speed of at least 1,000 km/s and even up to 2,000 km/s, which places it among the fastest EUV waves observed (Long et al, ; Liu et al, ). It propagated across the entire solar disk within half an hour starting from the eruption at 15:53 (Seaton & Darnel, ).…”

Section: The Flare Cmes and Gle 72: Close To The Sunmentioning

confidence: 95%

Modeling the Evolution and Propagation of 10 September 2017 CMEs and SEPs Arriving at Mars Constrained by Remote Sensing and In Situ Measurement

et al. 2018

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On 10 September 2017, solar energetic particles originating from the active region 12673 produced a ground level enhancement at Earth. The ground level enhancement on the surface of Mars, 160 longitudinally east of Earth, observed by the Radiation Assessment Detector (RAD) was the largest since the landing of the Curiosity rover in August 2012. Based on multipoint coronagraph images and the Graduated Cylindrical Shell model, we identify the initial 3-D kinematics of an extremely fast coronal mass ejection (CME) and its shock front, as well as another two CMEs launched hours earlier with moderate speeds. The three CMEs interacted as they propagated outward into the heliosphere and merged into a complex interplanetary CME (ICME). The arrival of the shock and ICME at Mars caused a very significant Forbush decrease seen by RAD only a few hours later than that at Earth, which was about 0.5 AU closer to the Sun. We investigate the propagation of the three CMEs and the merged ICME together with the shock, using the drag-based model and the WSA-ENLIL plus cone model constrained by the in situ observations. The synergistic study of the ICME and solar energetic particle arrivals at Earth and Mars suggests that to better predict potentially hazardous space weather impacts at Earth and other heliospheric locations for human exploration missions, it is essential to analyze (1) the eruption of the flare and CME at the Sun, (2) the CME kinematics, especially during their interactions, and (3) the spatially and temporally varying heliospheric conditions, such as the evolution and propagation of the stream interaction regions.Plain Language Summary From 4 to 6 September 2017, heliospheric activity suddenly and drastically increased starting from a simple sunspot which transformed into a complex region with four X-class flares accompanied by several Earth-directed magnetic clouds and shocks driven by them. Only a few days later, on 10 September 2017 starting at about 15:53, the same region launched another extremely fast magnetic cloud accompanied by an intense shock, which spread rapidly across the entire solar surface. Ten to 20 min later, particles accelerated at the Sun arrived at Earth, some of them with enough energy to reach Earth's surface and caused a ground level enhancement of radiation. A few hours later and shortly before 20:00, the Radiation Assessment Detector observed the biggest event since the landing of the Curiosity rover in August 2012 on the surface of Mars which was about 160 degrees east from Earth in the heliosphere. This was the first solar energetic particle event seen at ground level on the surface of two planets. Some particles were also transported across magnetic field lines throughout the heliosphere and were detected at the back side of the Sun where the eruption was centered. Meantime, the intense and wide shock also propagated into the interplanetary space, reached Earth on its west edge ∼50.5hr after launch and hit Mars on its east flank ∼59hr after launch, causing the biggest depression of the ...

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“…Perhaps the brightest and longest-lived plasma-sheet observation to date is associated with an X8.2-class flare on September 10th 2017 (e.g. Long et al 2018;Warren et al 2018;Kuridze et al 2019;Li et al 2018, Cheng et al 2018Longcope et al 2018;Gary et al 2018;Morosan et al 2019). The flare and coronal mass ejection erupted from AR 12673 on the western solar limb, observed across the spectrum by multiple spacebased and ground-based instruments.…”

Section: The Plasma-sheet Associated With the September 10th 2017 Flarementioning

confidence: 99%

Spectropolarimetric Insight into Plasma Sheet Dynamics of a Solar Flare

French

Judge

Matthews

et al. 2019

ApJL

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We examine spectropolarimetric data from the CoMP instrument, acquired during the evolution of the September 10th 2017 X8.2 solar flare on the western solar limb. CoMP captured linearly polarized light from two emission lines of Fe XIII at 1074.7 and 1079.8 nm, from 1.03 to 1.5 solar radii. We focus here on the hot plasma-sheet lying above the bright flare loops and beneath the ejected CME. The polarization has a striking and coherent spatial structure, with unexpectedly small polarization aligned with the plasma-sheet. By elimination, we find that small-scale magnetic field structure is needed to cause such significant depolarization, and suggest that plasmoid formation during reconnection (associated with the tearing mode instability) creates magnetic structure on scales below instrument resolution of 6 Mm. We conclude that polarization measurements with new coronagraphs, such as the upcoming DKIST, will further enhance our understanding of magnetic reconnection and development of turbulence in the solar corona.

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Plasma Evolution within an Erupting Coronal Cavity

Cited by 31 publications

References 35 publications

Microwave and Hard X-Ray Observations of the 2017 September 10 Solar Limb Flare

Microwave and Hard X-Ray Observations of the 2017 September 10 Solar Limb Flare

Modeling the Evolution and Propagation of 10 September 2017 CMEs and SEPs Arriving at Mars Constrained by Remote Sensing and In Situ Measurement

Spectropolarimetric Insight into Plasma Sheet Dynamics of a Solar Flare

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