2017
DOI: 10.1017/s1743921317009681
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Abstract: A characteristic pattern of solar hard X-ray emission, first identified in SOL1969-03-30 by Frost & Dennis (1971), turns out to have a close association with the prolonged high-energy gamma-ray emission originally observed by Forrestet al.(1985). This identification has become clear via the observations of long-duration γ-ray flares by theFermi/LAT experiment, for example in the event SOL2014-09-01. The distinctive features of these events include flat hard X-ray spectra extending well above 100 keV, a cha… Show more

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Cited by 10 publications
(12 citation statements)
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References 17 publications
(8 reference statements)
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“…This may be appropriate for some aspects of SEPs, as well as GCRs, given the likelihood that global coronal shock waves accelerate these particles. If this acceleration takes place on open fields, the SEPs that can return to the Sun and interact there may favor coronal holes (see Jin et al (2018) and Hudson (2018)). Of course the dominant γ-ray emission from solar flares also has a clear association with closed magnetic fields (Hurford et al 2003) associated with large sunspots.…”
Section: Discussionmentioning
confidence: 99%
“…This may be appropriate for some aspects of SEPs, as well as GCRs, given the likelihood that global coronal shock waves accelerate these particles. If this acceleration takes place on open fields, the SEPs that can return to the Sun and interact there may favor coronal holes (see Jin et al (2018) and Hudson (2018)). Of course the dominant γ-ray emission from solar flares also has a clear association with closed magnetic fields (Hurford et al 2003) associated with large sunspots.…”
Section: Discussionmentioning
confidence: 99%
“…However, after three hours, the region behind the blob will likely re-configure into a more dipole like structure. This would leave behind a large loop with seed particles, with those particles being unrelated to those in the impulsive phase, reminiscent of Hudson's lasso picture (Hudson 2018). ii.…”
Section: Discussionmentioning
confidence: 99%
“…Sep14 is the most intense and longest-lasting among the three behind-the-limb SGRE events observed by Fermi/LAT (Pesce-Rollins et al 2015a,b;Share et al 2018;Ackermann et al 2017;Plotnikov et al 2017;Jin et al 2018;Hudson 2018;Grechnev et al 2018). Plotnikov et al (2017), Ackermann et al (2017), and Share et al (2018) described the full time evolution of the SGRE flux.…”
Section: Data Descriptionmentioning
confidence: 99%
“…Open magnetic field lines (represented by the blue lines) in the sheath region that thread through the shock nose are rooted in the region beyond the dimming regions. Protons (>300 MeV, black coils) accelerated at the shock front travel along these open field lines precipitate to the solar chromosphere (indicated by the patches at the bottom of the blue lines) and produce γ-rays; the separation between the patches represents the largest spatial extent of the SGRE source.RecentlyHudson (2018) criticized the CME-shock solution by suggesting that a strong mirror force prevents protons from propagating sufficiently close to the Sun. The mirroring is a common problem to particles precipitating along any magnetic structure: PEA, flux rope, or the open structures threading the shock nose.…”
mentioning
confidence: 99%