Radio Imaging of a Type Ivm Radio Burst on the 14th of August 2010

Bain, H. M.; Krucker, S.; Saint-Hilaire, Pascal; Raftery, C. L.

doi:10.1088/0004-637x/782/1/43

Cited by 56 publications

(83 citation statements)

References 31 publications

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“…2). Gyro-synchrotron emission from electrons in the overlying flux rope was also reported in other events (Bastian et al 2001;Maia et al 2007;Bain et al 2014), but it can only be detected with imaging observations.…”

Section: An Interpretation Of Particle Acceleration During the Secondmentioning

confidence: 59%

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

Klein

Masson

Bouratzis

et al. 2014

A&A

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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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Section: An Interpretation Of Particle Acceleration During the Secondmentioning

confidence: 59%

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

Klein

Masson

Bouratzis

et al. 2014

A&A

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“…Park et al (2015) located the flare at N17°W52°, while Gopalswamy et al (2015) placed it at N12°W56°, both assigning it to NOAA Active Region (AR) 11099. On the other hand, Tun & Vourlidas (2013), Bain et al (2014), and Liewer et al (2015) associated it with AR 11093. In fact, AR 11099 was a new active region that appeared late on 2010 August 13 after the initially single sunspot of AR 11093 separated into two spots, helping to account for the uncertainty in the AR assignment.…”

Section: The Sep Event On 2010 August 14: Contextmentioning

confidence: 99%

“…Figure 5(b) shows a clear metric type II radio burst at frequencies ranging from ∼50 to 20 MHz starting at ∼09:52UT and lasting until 10:12 UT (Bain et al 2014). From fits to the type II burst emission, using the Newkirk (1961) and Baumbach-Allen radial density models, we find the burst was associated with a shock at heights between ∼1.25 and ∼1.95 R e , traveling at a speed of around 190-296 km s (e)) is not clearly observed.…”

Section: Solar Flarementioning

confidence: 99%

The Solar Energetic Particle Event of 2010 August 14: Connectivity with the Solar Source Inferred from Multiple Spacecraft Observations and Modeling

Lario

Kwon

Richardson

et al. 2017

ApJ

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We analyze one of the first solar energetic particle (SEP) events of solar cycle 24 observed at widely separated spacecraft in order to assess the reliability of models currently used to determine the connectivity between the sources of SEPs at the Sun and spacecraft in the inner heliosphere. This SEP event was observed on 2010 August 14 by near-Earth spacecraft, STEREO-A (∼80°west of Earth) and STEREO-B (∼72°east of Earth). In contrast to near-Earth spacecraft, the footpoints of the nominal magnetic field lines connecting STEREO-A and STEREO-B with the Sun were separated from the region where the parent fast halo coronal mass ejection (CME) originated by ∼88°and ∼47°in longitude, respectively. We discuss the properties of the phenomena associated with this solar eruption. Extreme ultraviolet and white-light images are used to specify the extent of the associated CME-driven coronal shock. We then assess whether the SEPs observed at the three heliospheric locations were accelerated by this shock or whether transport mechanisms in the corona and/or interplanetary space provide an alternative explanation for the arrival of particles at the poorly connected spacecraft. A possible scenario consistent with the observations indicates that the observation of SEPs at STEREO-B and near Earth resulted from particle injection by the CME shock onto the field lines connecting to these spacecraft, whereas SEPs reached STEREO-A mostly via cross-field diffusive transport processes. The successes, limitations, and uncertainties of the methods used to resolve the connection between the acceleration sites of SEPs and the spacecraft are evaluated.

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“…The cause of this type IV burst is believed to be the gyrosynchotron emission from the core of the CME, which corresponds to the erupting filament itself. Based on this observation, Tun & Vourlidas (2013) estimated the loop-top magnetic field strength along the line of sight and at 1 R above the solar surface to lie between 5 G and 15 G. Also assuming gyrosynchotron emission, Bain et al (2014) find lower magnetic field values of only several Gauss. This disagreement may be explained by the different choice of high-energy cutoff that was made in these studies (Bain et al 2014).…”

Section: Coronagraphmentioning

confidence: 97%

“…Based on this observation, Tun & Vourlidas (2013) estimated the loop-top magnetic field strength along the line of sight and at 1 R above the solar surface to lie between 5 G and 15 G. Also assuming gyrosynchotron emission, Bain et al (2014) find lower magnetic field values of only several Gauss. This disagreement may be explained by the different choice of high-energy cutoff that was made in these studies (Bain et al 2014). The short duration of an impulsive SEP event associated with a solar eruption is sometimes explained by assuming that these particles were accelerated at the flare site rather than at the CME shock front.…”

Section: Coronagraphmentioning

confidence: 97%

Solar signatures and eruption mechanism of the August 14, 2010 coronal mass ejection (CME)

D’Huys

Seaton

Groof

et al. 2017

J. Space Weather Space Clim.

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On August 14, 2010 a wide-angled coronal mass ejection (CME) was observed. This solar eruption originated from a destabilized filament that connected two active regions and the unwinding of this filament gave the eruption an untwisting motion that drew the attention of many observers. In addition to the erupting filament and the associated CME, several other low-coronal signatures that typically indicate the occurrence of a solar eruption were associated with this event. However, contrary to what was expected, the fast CME (v > 900 km s À1 ) was accompanied by only a weak C4.4 flare. We investigate the various eruption signatures that were observed for this event and focus on the kinematic evolution of the filament in order to determine its eruption mechanism. Had this solar eruption occurred just a few days earlier, it could have been a significant event for space weather. The risk of underestimating the strength of this eruption based solely on the C4.4 flare illustrates the need to include all eruption signatures in event analyses in order to obtain a complete picture of a solar eruption and assess its possible space weather impact.

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Radio Imaging of a Type Ivm Radio Burst on the 14th of August 2010

Cited by 56 publications

References 31 publications

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

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

The Solar Energetic Particle Event of 2010 August 14: Connectivity with the Solar Source Inferred from Multiple Spacecraft Observations and Modeling

Solar signatures and eruption mechanism of the August 14, 2010 coronal mass ejection (CME)

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