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Wills-Davey, M. J.; Thompson, B. J.

doi:10.1023/a:1005201500675

Cited by 167 publications

(127 citation statements)

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“…The clear answer is to apply the Huygens principle to the observations to seek information about the nature of the wave radiant source (Wills-Davey and Thompson 1999;Khan and Aurass 2002;Temmer et al 2009). It is limited by the resolution and sensitivity of the observations in several ways, but in principle Huygens reconstructions can give us key information about the shape, location, and activation time of the actual region of magnetic energy release.…”

Section: Wave Synthesis: the Huygens Principlementioning

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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Section: Wave Synthesis: the Huygens Principlementioning

confidence: 99%

Global Properties of Solar Flares

2011

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“…The phenomenon of '' sympathetic flaring '' (Richardson 1951;Becker 1958;Valniček 1964;Wang et al 2001) has recently been revisited by Biesecker & Thompson (2000), who demonstrated that there is no appreciable increase in the frequency of solar flares following the propagation of an EIT wave. The sympathetic flaring study was prompted by the observation of the EIT waves' long duration and far propagation and by observations that the EIT wave produces visible deflections in the ambient corona as it propagates Wills-Davey & Thompson 1999). However, the Biesecker & Thompson (2000) study is limited by the small number of on-disk waves analyzed (31) and the relatively low cadence of the EIT images (7-15 minutes per image).…”

Section: Introductionmentioning

confidence: 99%

Interaction of EIT Waves with Coronal Active Regions

Ofman

Thompson

2002

ApJ

179

168

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Large-scale coronal waves associated with flares were first observed by the Solar and Heliospheric Observatory (SOHO) Extreme ultraviolet Imaging Telescope (EIT). We present the first three-dimensional MHD modeling of the interaction of the EIT waves with active regions and the possibility of destabilization of an active region by these waves. The active region is modeled by an initially force-free, bipolar magnetic configuration with gravitationally stratified density. We include finite thermal pressure and resistive dissipation in our model. The EIT wave is launched at the boundary of the region, as a short time velocity pulse that travels with the local fast magnetosonic speed toward the active region. We find that the EIT wave undergoes strong reflection and refraction, in agreement with observations, and induces transient currents in the active region. The resulting Lorentz force leads to the dynamic distortion of the magnetic field and to the generation of secondary waves. The resulting magnetic compression of the plasma induces flows, which are particularly strong in the current-carrying active region. We investigate the effect of the magnetic field configuration and find that the current-carrying active region is destabilized by the impact of the wave. Analysis of the threedimensional interaction between EIT waves and active regions can serve as a diagnostic of the active region coronal magnetic structure and stability.

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“…On the large scale, flares are associated with fast coronal waves (EUV and Moreton waves) and coronal mass ejection (CME) into interplanetary space (Moreton & Ramsey 1960;Thompson et al 1999;Wills-Davey & Thompson 1999;Klassen et al 2000). The link between the local, rapid brightenings and the larger scale CMEs is a question of some debate (Kahler 1992;Harrison 1995;Nitta & Akiyama 1999).…”

Section: Introductionmentioning

confidence: 99%

Large Doppler Shifts in X-Ray Plasma: An Explosive Start to Coronal Mass Ejection

Innes

Curdt

Schwenn

et al. 2001

The Astrophysical Journal

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We report observations, taken with the Solar Ultraviolet Measurements of Emitted Radiation spectrometer, of spatially resolved high red and blue Doppler shifts (up to 650 km s ) from X-ray-emitting plasma in the corona Ϫ1 above a flare. The high Doppler shifts are seen minutes after a fast, faint optical front is seen racing through the same part of the corona in images taken with the Mirror Coronagraph for Argentina. The association of the largescale fast optical emission front with soft X-ray emission and high Doppler shifts suggests plasma heating and acceleration in the wake of a shock.

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Cited by 167 publications

References 0 publications

Global Properties of Solar Flares

Global Properties of Solar Flares

Interaction of EIT Waves with Coronal Active Regions

Large Doppler Shifts in X-Ray Plasma: An Explosive Start to Coronal Mass Ejection

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