Acceleration in Fast Halo CMEs and Synchronized Flare HXR Bursts

Temmer, Manuela; Veronig, Astrid; Vršnak, Bojan; Rybák, J.; Gömöry, P.; Stoiser, Sigrid; Maričić, Darije

doi:10.1086/527414

Cited by 203 publications

(196 citation statements)

References 44 publications

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“…Recently, based on a number of CMEs observed by the C1, C2, and C3 telescopes of Large Angle and Spectrometric Coronagraph (LASCO) for which the initial acceleration was adequately resolved, the "acceleration phase" of these CME events was empirically found to coincide with the rise phase of the associated flare X-ray emission (Zhang et al 2001). This finding has been supported by recent work of Maričič et al (2007) and Temmer et al (2008). They, however, also discovered exceptions and considerable scatter in the timing correlation.…”

Section: Introductionsupporting

confidence: 68%

Temporal and Physical Connection Between Coronal Mass Ejections and Flares

Chen

Kunkel

2010

ApJ

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The physical connection between the eruption of coronal mass ejections (CMEs) and associated flare energy release is examined. The trajectories of five CMEs are determined using LASCO/SOHO or SECCHI/STEREO data, and the associated soft X-ray (SXR) light curves are obtained from GOES 1-8 Å data. As the theoretical description of CME physics, the existing erupting flux-rope model is used in which an initial flux rope is driven out of equilibrium by the increasing poloidal magnetic flux Φ p (t) (poloidal "flux injection"). Mathematically, this is represented by dΦ p (t)/dt. For each CME, this function is adjusted to obtain the solution that best fits the observed height-time data. The resulting dΦ p (t)/dt is shown to be strongly constrained by the CME height data. This function and the attendant electromotive force (EMF) given by E(t) ≡ −(1/c)dΦ p (t)/dt constitute predictions of the theory for each CME trajectory. It is shown that the best-fit solutions fit the CME trajectories within 1%-2% of the CME height data and that the temporal profile of the predicted dΦ p (t)/dt is correlated with that of the associated X-ray light curve regardless of the flare duration. Specifically, we find that the observed duration of SXR emission ΔT SXR is comparable to and scales with the predicted duration ΔT p of poloidal flux injection, i.e., ΔT SXR ΔT p . Neither the predicted dΦ p (t)/dt nor the input CME height data contain any information on X-ray data. Thus, the correlation is nontrivial, constituting evidence that poloidal flux injection is physically connected to flare energy release. It is suggested that this connection is provided by the EMF that produces electric fields to accelerate particles.

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Section: Introductionsupporting

confidence: 68%

Temporal and Physical Connection Between Coronal Mass Ejections and Flares

Chen

Kunkel

2010

ApJ

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“…However, it has been shown that the acceleration profile of CMEs tends to peak during this period, too (cf. Zhang et al, 2001;Maričić et al, 2007;Temmer et al, 2008;Berkebile-Stoiser et al, 2012). Since coronal waves are highly associated with CMEs too (Section 5.2), timing alone cannot be used to make a distinction between a flare-related and a CME-related wave launch mechanism.…”

Section: Solar Flaresmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

163

140

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Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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“…Though, the flare impulsive phase is often closely associated with the acceleration phase of the flare-related CMEs [173][174][175].…”

Section: Volume 35mentioning

confidence: 99%

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Hamidi

2014

ILCPA

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The solar flare and Coronal Mass Ejections (CMEs) are well known as one of the most massive eruptions which potentially create major disturbances in the interplanetary medium and initiate severe magnetic storms when they collide with the Earth's magnetosphere. However, how far the solar flare can contribute to the formation of the CMEs is still not easy to be understood. These phenomena are associated with II and III burst it also divided by sub-type of burst depending on the physical characteristics and different mechanisms. In this work, we used a Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy in Transportable Observatories (CALLISTO) system. The aim of the present study is to reveal dynamical properties of solar burst type II and III due to several mechanisms. Most of the cases of both solar radio bursts can be found in the range less that 400 MHz. Based on solar flare monitoring within 24 hours, the CMEs that has the potential to explode will dominantly be a class of M1 solar flare. Overall, the tendencies of SRBT III burst form the solar radio burst type III at 187 MHz to 449 MHz. Based on solar observations, it is evident that the explosive, short time-scale energy release during flares and the long term, gradual energy release expressed by CMEs can be reasonably understood only if both processes are taken as common and probably not independent signatures of a destabilization of pre-existing coronal magnetic field structures. The configurations of several active regions can be sourced regions of CMEs formation. The study of the formation, acceleration and propagation of CMEs requires advanced and powerful observational tools in different spectral ranges as many 'stages' as possible between the photosphere of the Sun and magnetosphere of the Sun and magnetosphere of the Earth. In conclusion, this range is a current regime of solar radio bursts during CMEs events.

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Acceleration in Fast Halo CMEs and Synchronized Flare HXR Bursts

Cited by 203 publications

References 44 publications

Temporal and Physical Connection Between Coronal Mass Ejections and Flares

Temporal and Physical Connection Between Coronal Mass Ejections and Flares

Large-scale Globally Propagating Coronal Waves

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

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