Hard X-ray emission from a flare-related jet

Bain, H. M.; Fletcher, L.

doi:10.1051/0004-6361/200911876

Cited by 38 publications

(40 citation statements)

References 34 publications

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“…We choose p to vary between 6 and 16. This range is suggested by recent observations of X‐rays associated with type III bursts [ Krucker et al , ; Bain and Fletcher , ; Glesener et al , ]. It is also used in previous modeling for type III bursts [ Harvey , ], for both type III bursts and X‐rays [ Reid et al , ], and for Langmuir waves in the lower corona [ Zharkova and Siversky , ].…”

Section: Scalings With the Parameters Of Power Law Injectionmentioning

confidence: 98%

Type III bursts produced by power law injected electrons in Maxwellian background coronal plasmas

Cairns

2013

JGR Space Physics

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[1] Simulations are presented for coronal type III bursts produced by injection of energetic electrons with power law speed spectra onto open magnetic field lines embedded in an otherwise unmagnetized Maxwellian background coronal plasma, including quasi-linear wave-particle interactions and nonlinear wave-wave processes. The simulations show that although fast electrons with speeds > 0.3c are injected, they are important only to the onset and not to the peak of f p emission, where f p is the local electron plasma frequency. Instead, slower beam electrons are the major drivers of the peak f p emission. Therefore, the type III beam speeds derived from the drift rates of peak f p emission are less than the typical speeds of c/3 observed for coronal type III bursts. This occurs mainly because the number of fast beam electrons with speeds > 0.3c is much less than the slower ones, causing weaker f p emission from these fast beam electrons. Comparisons are made with injected electrons having Maxwellian spectra. We find that type III beams are faster when the injection has power law spectra, since there are more fast electrons injected than for Maxwellian spectra. These results suggest that type III beams produced in the corona with Maxwellian background particle distributions and either power law or Maxwellian spectra can account only for the lower half of the observed range 0.1-0.6c of type III beam speeds but not for the upper half.Citation: Li, B., and I. H. Cairns (2013), Type III bursts produced by power law injected electrons in Maxwellian background coronal plasmas,

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Section: Scalings With the Parameters Of Power Law Injectionmentioning

confidence: 98%

Type III bursts produced by power law injected electrons in Maxwellian background coronal plasmas

Cairns

2013

JGR Space Physics

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“…The duration of the impulse matters, because the detection sensitivity for helioseismic waves depends upon the temporal frequency (and resulting spatial structure) of the photospheric ripples. Seismic wave e 40 20-50 2.5 × 10 22 a Bain and Fletcher (2009) b Alfvénic c Rough estimate d Canfield et al (1987) e 10 29 erg…”

Section: Seismic Wavesmentioning

confidence: 99%

Global Properties of Solar Flares

2011

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This article broadly reviews our knowledge of solar flares. There is a particular focus on their global properties, as opposed to the microphysics such as that needed for magnetic reconnection or particle acceleration as such. Indeed solar flares will always remain in the domain of remote sensing, so we cannot observe the microscales directly and must understand the basic physics entirely via the global properties plus theoretical inference. The global observables include the general energetics-radiation in flares and mass loss in coronal mass ejections (CMEs)-and the formation of different kinds of ejection and global wave disturbance: the type II radio-burst exciter, the Moreton wave, the EIT "wave", and the "sunquake" acoustic waves in the solar interior. Flare radiation and CME kinetic energy can have comparable magnitudes, of order 10 32 erg each for an X-class event, with the bulk of the radiant energy in the visible-UV continuum. We argue that the impulsive phase of the flare dominates the energetics of all of these manifestations, and also point out that energy and momentum in this phase largely reside in the electromagnetic field, not in the observable plasma.

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“…Many papers report a significant delay between jet formation and flux emergence in contrast to recent 3D Early observations of X-ray jets associated with bursts of metric radio emission implied that the jet mechanism was able to accelerate sub-relativistic electrons along dense corona structures (Aurass et al 1994;Kundu et al 1995;Raulin et al 1996). Further confirmation came from observations of jets which were co-incident with hard X-rays from their footpoints (Chen et al 2013;Krucker et al 2011;Nitta 1997;Nitta et al 2008) and from the jet itself (Bain & Fletcher 2009;Glesener et al 2012).…”

Section: Introductionmentioning

confidence: 98%

Observations of solar X‐ray and EUV jets and their related phenomena

et al. 2016

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Solar jets are fast‐moving, elongated brightenings related to ejections seen in both images and spectra on all scales from barely visible chromospheric jets to coronal jets extending up to a few solar radii. The largest, most powerful jets are the source of type III radio bursts, energetic electrons and ions with greatly enhanced 3He and heavy element abundances. The frequent coronal jets from polar and equatorial coronal holes may contribute to the solar wind. The primary acceleration mechanism for all jets is believed to be release of magnetic stress via reconnection; however the energy buildup depends on the jets' source environment. In this review, we discuss how certain features of X‐ray and EUV jets, such as their repetition rate and association with radio emission, depends on their underlying photospheric field configurations (active regions, polar and equatorial coronal holes, and quiet Sun). (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Hard X-ray emission from a flare-related jet

Cited by 38 publications

References 34 publications

Type III bursts produced by power law injected electrons in Maxwellian background coronal plasmas

Type III bursts produced by power law injected electrons in Maxwellian background coronal plasmas

Global Properties of Solar Flares

Observations of solar X‐ray and EUV jets and their related phenomena

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