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Reconnection in the Post-Impulsive Phase of Solar Flares  

Dan Seaton   Submitted: 2018-04-02 22:11

Using a recently developed analytical procedure, we determine the rate of magnetic reconnection in the "standard" model of eruptive solar flares. During the late phase, the neutral line is located near the lower tip of the reconnection current sheet, and the upper region of the current sheet is bifurcated into a pair of Petschek-type shocks. Despite the presence of these shocks, the reconnection rate remains slow if the resistivity is uniform and the flow is laminar. Fast reconnection is achieved only if there is some additional mechanism that can shorten the length of the diffusion region at the neutral line. Observations of plasma flows by the X-Ray Telescope (XRT) on Hinode imply that the diffusion region is in fact quite short. Two possible mechanisms for reducing the length of the diffusion region are localized resistivity and MHD turbulence.

Authors: Terry G. Forbes, Daniel B. Seaton, Katharine K. Reeves
Projects: None

Publication Status: Accepted to ApJ
Last Modified: 2018-04-04 12:18
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Observations of an Eruptive Solar Flare in the Extended EUV Solar Corona  

Dan Seaton   Submitted: 2017-12-21 21:34

We present observations of a powerful solar eruption, accompanied by an X8.2 solar flare, from NOAA Active Region 12673 on 2017 September 10 by the Solar Ultraviolet Imager (SUVI) on the GOES-16 spacecraft. SUVI is noteworthy for its relatively large field of view, which allows it to image solar phenomena to heights approaching 2 solar radii. These observations include the detection of an apparent current sheet associated with magnetic reconnection in the wake of the eruption and evidence of an extreme-ultraviolet wave at some of the largest heights ever reported. We discuss the acceleration of the nascent coronal mass ejection to approximately 2000 km s-1 at about 1.5 solar radii. We compare these observations with models of eruptions and eruption-related phenomena. We also describe the SUVI data and discuss how the scientific community can access SUVI observations of the event.

Authors: Daniel B. Seaton and Jonathan M. Darnel
Projects: GOES/SUVI

Publication Status: ApJL (In press)
Last Modified: 2018-01-03 11:41
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Solar signatures and eruption mechanism of the 2010 August 14 CME  

Dan Seaton   Submitted: 2017-02-06 13:45

On 2010 August 14, a wide-angled coronal mass ejection (CME) was observed. This solar eruption originated from a destabilized filament that connected two active regions and the unwinding of this filament gave the eruption an untwisting motion that drew the attention of many observers. In addition to the erupting filament and the associated CME, several other low-coronal signatures that typically indicate the occurrence of a solar eruption were associated to this event. However, contrary to what is expected, the fast CME (v>900 km s-1) was accompanied by only a weak C4.4 flare. We investigate the various eruption signatures that were observed for this event and focus on the kinematic evolution of the filament in order to determine its eruption mechanism. Had this solar eruption occurred just a few days earlier, it could have been a significant event for space weather. The risk to underestimate the strength of this eruption based solely on the C4.4 flare illustrates the need to include all eruption signatures in event analyses in order to obtain a complete picture of a solar eruption and assess its possible space weather impact.

Authors: Elke D'Huys, Daniel B. Seaton, Anik De Groof, David Berghmans, Stefaan Poedts
Projects: ACE,GOES X-rays,PROBA2/SWAP,SDO-AIA,SDO-HMI,SoHO-LASCO,STEREO

Publication Status: Accepted for publication in the Journal of Space Weather and Space Climate
Last Modified: 2017-02-07 23:56
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Abstracts by Author
Reconnection in the Post-Impulsive Phase of Solar Flares
Observations of an Eruptive Solar Flare in the Extended EUV Solar Corona
Solar signatures and eruption mechanism of the 2010 August 14 CME

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