Solar source of energetic particles in interplanetary space during the 2006 December 13 event

Li, C.; Dai, Y.; Vial, J. C.; Owen, C. J.; Matthews, Sarah; Tang, Yuhua; Fang, Cheng; Fazakerley, A. N.

doi:10.1051/0004-6361/200911986

Cited by 29 publications

(23 citation statements)

References 73 publications

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“…There have already been detailed studies in literature concerning characteristics and physical processes linked to SPEs (Cliver et al 1982;Kahler 1994;Mewaldt et al 2005;Tylka et al 2005, and more recently from Reames 2009& Li et al 2009). Similar studies concerning specific SPEs detected by SREM units will be the subject of forthcoming papers, as this is an ongoing research.…”

Section: Introductionmentioning

confidence: 99%

Using a new set of space-borne particle monitors to investigate solar-terrestrial relations

Tziotziou

Sandberg

Anastasiadis

et al. 2010

A&A

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Context. We investigated the solar origin of Solar Particle Events (SPEs) which occurred during four time periods of the 23rd solar cycle with intense solar activity and were detected by the Standard Radiation Environment Monitor (SREM) onboard the INTEGRAL satellite. SREM is a second generation ESA particle radiation monitor, already flying onboard seven spacecraft. Aims. The present study attempts to establish the association of recorded SPEs by INTEGRAL/SREM with their solar sources and hence evaluate the potential of SREM units as an alarm system for hazardous SPEs. Methods. X-ray, optical and radio data of solar flares and coronal mass ejections (CMEs) that were observed by several space-based instruments during the aforementioned solar cycle were reduced and thoroughly analyzed to establish the corresponding solar origin of the selected SPEs. Conclusions. SREM proves to be a new valuable asset for a comprehensive study of SPEs and a useful alert instrument for explosive geoeffective solar events.

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Section: Introductionmentioning

confidence: 99%

Using a new set of space-borne particle monitors to investigate solar-terrestrial relations

Tziotziou

Sandberg

Anastasiadis

et al. 2010

A&A

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“…We then use the PFSS model developed by Schrijver & DeRosa (2003), which is available in the IDL-based solar software (SSW) package, to identify the coronal magnetic configurations. It has been successfully applied in relating the large-scale topologies to the coronal plasma outflows (Sakao et al 2007) and to the open field-line fluxes (Li et al 2009). Using the photospheric longitudinal magnetogram from the Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory (SOHO), the coronal magnetic configuration of each event is extrapolated.…”

Section: Discussionmentioning

confidence: 99%

Major Electron Events and Coronal Magnetic Configurations of the Related Solar Active Regions

Owen

Matthews

et al. 2010

ApJ

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A statistical survey of 26 major electron events during the period 2002 February through the end of solar cycle 23 is presented. We have obtained electron solar onset times and the peak flux spectra for each event by fitting to a power-law spectrum truncated by an exponential high-energy tail, i.e., f (E) ∼ E −δ e −E/E 0 . We also derived the coronal magnetic configurations of the related solar active regions (ARs) from the potential-field source-surface (PFSS) model. It is found that: (1) 10 of the 11 well-connected open field-line events are prompt events whose solar onset times coincide with the maxima of flare emission. 13 of the 14 closed field-line events are delayed events. (2) A not-well-connected open field-line event and one of the closed field-line events are prompt events, they are both associated with large-scale coronal disturbances or dimming. (3) An averaged harder spectrum is found in open field-line events compared with the closed ones. Specifically, the averaged spectral index δ is of 1.6 ± 0.3 in open field-line events and of 2.0 ± 0.4 in closed ones. The spectra of three closed fieldline events show infinite rollover energies E 0 . These correlations clearly establish a significant link between the coronal magnetic field-line topology and the escape of charged particles from the flaring ARs into interplanetary space during the major solar energetic particle (SEP) events.

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“…For the flares producing IT3 but without CMEs, it is suspected that their source regions are already close to the open flux so that no further interchange reconnection is required. In this case, accelerated electrons can escape easily to the interplanetary space along the open flux, producing the IT3 (e.g., Li et al 2009;Krucker et al 2011;Chen et al 2018;Glesener & Fleishman 2018). Statistically, the former scenario seems to occur slightly more frequently than the latter one, as evidenced by the proportion of 58% for CME-associated flares vs. 41% for CME-less flares that are accompanied by IT3.…”

Section: Correlation Of Cmes To Interplanetary Type III Burstsmentioning

confidence: 99%

What determine Solar Flares Producing Interplanetary Type III Radio Bursts?

Kou,

Jing,

Cheng

et al. 2020

Preprint

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Energetic electrons accelerated by solar flares often give rise to type III radio bursts at a broad waveband and even interplanetary type III bursts (IT3) if the wavelength extends to decameter-kilometer. In this Letter, we investigate the probability of the flares that produce IT3, based on the sample of 2272 flares above M-class observed from 1996 to 2016. It is found that only 49.6% of the flares are detected to be accompanied with IT3. The duration, peak flux, and fluence of the flares with and without IT3 both present power-law distributions in the frequency domain, but the corresponding spectral indices for the former (2.06±0.17, 2.04±0.18, and 1.55±0.09) are obviously smaller than that for the latter (2.82±0.22, 2.51±0.19, and 2.40±0.09), showing that the flares with IT3 have longer durations and higher peak fluxes. We further examine the relevance of coronal mass ejections (CMEs) to the two groups of flares. It is found that 58% (655 of 1127) of the flares with IT3 but only 19% (200 of 1078) of the flares without IT3 are associated with CMEs, and that the associated CMEs for the flares with IT3 are inclined to be wider and faster. This indicates that CMEs may also play a role in producing IT3, speculatively facilitating the escape of accelerated electrons from the low corona to the interplanetary space.

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Solar source of energetic particles in interplanetary space during the 2006 December 13 event

Cited by 29 publications

References 73 publications

Using a new set of space-borne particle monitors to investigate solar-terrestrial relations

Using a new set of space-borne particle monitors to investigate solar-terrestrial relations

Major Electron Events and Coronal Magnetic Configurations of the Related Solar Active Regions

What determine Solar Flares Producing Interplanetary Type III Radio Bursts?

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