Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Miteva, R.; Klein, Karl‐Ludwig; Kienreich, I. W.; Temmer, Manuela; Veronig, Astrid; Malandraki, O.

doi:10.1007/s11207-014-0499-5

Cited by 44 publications

(53 citation statements)

References 51 publications

(69 reference statements)

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“…For those events which had an associated type II radio burst, the start of the radio emission was observed after the start of the wave in the vast majority of cases (see Figure 6a), similar to the relative start times of waves and radio bursts reported by Miteva et al (2014) and Warmuth (2010). This delay between the start time of the global wave and the associated type II burst is likely due to the time taken for the disturbance to either become superAlfvénic (as modelled by Vršnak and Lulić, 2000), or the time taken for the driver to reach regions of low ambient Alfvén speed in the corona (Mann et al, 2003;Zucca et al, 2014); in some cases this can take up to 30 minutes after detection of the wave.…”

Section: Relationship With Type II Radio Burstssupporting

confidence: 79%

“…A window 90 minutes either side of the start time of the global wave was used to look for associated events in the NOAA/SWPC list. This choice of time window was motivated by the fact that type II radio bursts can be seen up to 15 minutes before or after the first instance of an EUV wave observation (Park et al, 2013;Warmuth, 2010;Miteva et al, 2014); the larger time window used here was chosen to account for any anomalous events. For each candidate radio burst associated with a global wave, the SWPC list provides an associated start time, an end time, the observatory used to make the observation, the frequency range of the burst and the estimated drift speed.…”

Section: Identification and Characterisation Of Type II Radio Burstsmentioning

confidence: 99%

“…Rouillard et al, 2012;Prise et al, 2014). This approach was also used by Miteva et al (2014) to study 179 SEP events between 1997 and 2006, finding that protons detected in situ were related to the global EUV waves, but that there was no correlation between the waves and electrons.…”

Section: Introductionmentioning

confidence: 99%

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A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves

et al. 2017

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Solar eruptions are the most spectacular events in our solar system and are associated with many different signatures of energy release including solar flares, coronal mass ejections, global waves, radio emission and accelerated particles. Here, we apply the Coronal Pulse Identification and Tracking Algorithm (CorPITA) to the high-cadence synoptic data provided by the Solar Dynamics Observatory (SDO) to identify and track global waves observed by SDO. 164 of the 362 solar flare events studied (45%) were found to have associated global waves with no waves found for the remaining 198 (55%). A clear linear relationship was found between the median initial velocity and the acceleration of the waves, with faster waves exhibiting a stronger deceleration (consistent with previous results). No clear relationship was found between global waves and type II radio bursts, electrons or protons detected in situ near Earth. While no relationship was found between the wave properties and the associated flare size (with waves produced by flares from B to X-class), more than a quarter of the active regions studied were found to produce more than one wave event. These results suggest that the presence of a global wave in a solar eruption is most likely determined by the structure and connectivity of the erupting active region and the surrounding quiet solar corona rather than by the amount of free energy available within the active region.

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Section: Relationship With Type II Radio Burstssupporting

confidence: 79%

Section: Identification and Characterisation Of Type II Radio Burstsmentioning

confidence: 99%

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A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves

et al. 2017

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“…The largest statistical study of wave-associated SEPs was undertaken by Miteva et al (2014), who analyzed 179 SEP events and found that 87% of them were accompanied by EIT waves. In events with no apparent magnetic connection to Earth, the waves' arrival time at the footpoint of the Parker spiral showed a significant correlation with the extrapolated injection times of IP protons.…”

Section: Acceleration Of Solar Energetic Particles (Seps)mentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

156

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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“…3.2. The 2005 Jan. 20 event was clearly eruptive, with a fast CME (Grechnev et al 2008) and an EUV wave (Miteva et al 2014). These phenomena were very likely accompanied by shock waves and therefore Type II radio bursts.…”

Section: Relativistic Proton Release and Electromagnetic Emissionsmentioning

confidence: 99%

The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration

Klein

Masson

Bouratzis

et al. 2014

A&A

Self Cite

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Context. The highest energies of solar energetic nucleons detected in space or through gamma-ray emission in the solar atmosphere are in the GeV range. Where and how the particles are accelerated is still controversial. Aims. We search for observational information on the location and nature of the acceleration region(s) by comparing the timing of relativistic protons detected on Earth and radiative signatures in the solar atmosphere during the particularly well-observed 2005 Jan. 20 event.Methods. This investigation focusses on the post-impulsive flare phase, where a second peak was observed in the relativistic proton time profile by neutron monitors. This time profile is compared in detail with UV imaging and radio spectrography over a broad frequency band from the low corona to interplanetary space. Results. It is shown that the late relativistic proton release to interplanetary space was accompanied by a distinct new episode of energy release and electron acceleration in the corona traced by the radio emission and by brightenings of UV kernels. These signatures are interpreted in terms of magnetic restructuring in the corona after the coronal mass ejection passage. Conclusions. We attribute the delayed relativistic proton acceleration to magnetic reconnection and possibly to turbulence in largescale coronal loops. While Type II radio emission was observed in the high corona, no evidence of a temporal relationship with the relativistic proton acceleration was found.

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Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Cited by 44 publications

References 51 publications

A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves

A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves

Large-scale Globally Propagating Coronal Waves

The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration

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