Probing the Puzzle of Behind-the-limb γ-Ray Flares: Data-driven Simulations of Magnetic Connectivity and CME-driven Shock Evolution

Jin, Meng; Petrosian, V.; Liu, W.; Nitta, N.; Omodei, N.; Costa, Fatima Rubio da; Effenberger, Frederic; Li, Gang; Pesce-Rollins, M.; Allafort, A.; Manchester, W.

doi:10.3847/1538-4357/aae1fd

Cited by 40 publications

(40 citation statements)

References 78 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This means the western edge of the flux rope extends to the frontside of the Sun. The shock, which is more extended than the flux rope, clearly extends to the frontside and is consistent with the EUV wave crossing the STB west limb and propagating to the frontside (Plotnikov et al 2017;Jin et al 2018). In the case of high-inclination flux ropes, the east-west extent would be smaller and a source at 40⁰ behind the limb may not produce a γray event on the Earth-facing disk.…”

Section: The Cme and Shocksupporting

confidence: 69%

“…We make use of the fact that the type II radio burst was observed by SWAVES without obstruction, so we obtain the full evolution of the burst in the radio dynamic spectrum. The early phase of the shock has already been described in previous papers (Plotnikov et al 2017;Jin et al 2018;Grechnev et al 2018). Here we provide information on the shock and CME as observed by the Large Angle and Spectrometric Coronagraph (LASCO, Brueckner et al 1995) on board SOHO and the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI, ) on board STEREO.…”

Section: Data Descriptionsupporting

confidence: 58%

“…Sep14 is the most intense and longest-lasting among the three behind-the-limb SGRE events observed by Fermi/LAT (Pesce-Rollins et al 2015a,b;Share et al 2018;Ackermann et al 2017;Plotnikov et al 2017;Jin et al 2018;Hudson 2018;Grechnev et al 2018). Plotnikov et al (2017), Ackermann et al (2017), and Share et al (2018) described the full time evolution of the SGRE flux.…”

Section: Data Descriptionmentioning

confidence: 99%

“…The Sep14 SGRE event originated from an active region located ~37⁰ behind the east limb (N14E127 -see Ackermann et al 2017;Plotnikov et al 2017;Jin et al 2018;Grechnev et al 2018). Fortunately, there were three space observatories in which the source was observed as a frontside event (see Fig.…”

Section: The Solar Sourcementioning

confidence: 99%

“…Cliver et al (1993) were cautious to state that it was an open question whether shock mechanism applicable to GRL emission would also apply to SGREs. The observation of SGRE from three backside events by Fermi/LAT provided definite evidence that the time-extended emission is also spatially extended (Pesce-Rollins et al 2015a,b;Plotnikov et al 2017;Ackerman et al 2017;Jin et al 2018). In particular, the SOL2014-09-01 (Sep14, for short) event was extraordinary in that the eruption was ~ 40⁰ behind the limb, yet SGRE was observed by Fermi/LAT suggesting that the SGRE emission is truly spatially extended and must be due to a CME-driven shock.…”

mentioning

confidence: 98%

See 4 more Smart Citations

Source of Energetic Protons in the 2014 September 1 Sustained Gamma-ray Emission Event

et al. 2020

View full text Add to dashboard Cite

We report on the source of >300 MeV protons during the SOL2014-09-01 sustained gamma-ray emission (SGRE) event based on multi-wavelength data from a wide array of space-and groundbased instruments. Based on the eruption geometry we provide concrete explanation for the spatially and temporally extended γ-ray emission from the eruption. We show that the associated flux rope is of low inclination (roughly oriented in the east-west direction), which enables the associated shock to extend to the frontside. We compare the centroid of the SGRE source with the location of the flux rope's leg to infer that the high-energy protons must be precipitating between the flux rope leg and the shock front. The durations of the SOL2014-09-01 SGRE event and the type II radio burst agree with the linear relationship between these parameters obtained for other SGRE events with duration ≥3 hrs. The fluence spectrum of the SEP event is very hard, indicating the presence of high-energy (GeV) particles in this event. This is further confirmed by the presence of an energetic coronal mass ejection (CME) with a speed >2000 km/s, similar to those in ground level enhancement (GLE) events. The type II radio burst had emission components from metric to kilometric wavelengths as in events associated with GLE events. All these factors indicate that the high-energy particles from the shock were in sufficient numbers needed for the production of γ-rays via neutral pion decay.

show abstract

Section: The Cme and Shocksupporting

confidence: 69%

Section: Data Descriptionsupporting

confidence: 58%

Section: Data Descriptionmentioning

confidence: 99%

Section: The Solar Sourcementioning

confidence: 99%

mentioning

confidence: 98%

See 3 more Smart Citations

Source of Energetic Protons in the 2014 September 1 Sustained Gamma-ray Emission Event

et al. 2020

View full text Add to dashboard Cite

show abstract

The high-energy Sun - probing the origins of particle acceleration on our nearest star

Matthews¹,

Reid²,

Baker³

et al. 2021

Exp Astron

Self Cite

View full text Add to dashboard Cite

As a frequent and energetic particle accelerator, our Sun provides us with an excellent astrophysical laboratory for understanding the fundamental process of particle acceleration. The exploitation of radiative diagnostics from electrons has shown that acceleration operates on sub-second time scales in a complex magnetic environment, where direct electric fields, wave turbulence, and shock waves all must contribute, although precise details are severely lacking. Ions were assumed to be accelerated in a similar manner to electrons, but γ-ray imaging confirmed that emission sources are spatially separated from X-ray sources, suggesting distinctly different acceleration mechanisms. Current X-ray and γ-ray spectroscopy provides only a basic understanding of accelerated particle spectra and the total energy budgets are therefore poorly constrained. Additionally, the recent detection of relativistic ion signatures lasting many hours, without an electron counterpart, is an enigma. We propose a single platform to directly measure the physical conditions present in the energy release sites and the environment in which the particles propagate and deposit their energy. To address this fundamental issue, we set out a suite of dedicated instruments that will probe both electrons and ions simultaneously to observe; high (seconds) temporal resolution photon spectra (4 keV – 150 MeV) with simultaneous imaging (1 keV – 30 MeV), polarization measurements (5–1000 keV) and high spatial and temporal resolution imaging spectroscopy in the UV/EUV/SXR (soft X-ray) regimes. These instruments will observe the broad range of radiative signatures produced in the solar atmosphere by accelerated particles.

show abstract

Localization of the Gamma-Ray Emission Region in the 1 September 2014 Behind-the-Limb Solar Flare According to the Fermi/LAT Data

Kochanov,

Kiselev,

Grechnev

et al. 2024

Sol Phys

View full text Add to dashboard Cite

Probing the Puzzle of Behind-the-limb γ-Ray Flares: Data-driven Simulations of Magnetic Connectivity and CME-driven Shock Evolution

Cited by 40 publications

References 78 publications

Source of Energetic Protons in the 2014 September 1 Sustained Gamma-ray Emission Event

Source of Energetic Protons in the 2014 September 1 Sustained Gamma-ray Emission Event

The high-energy Sun - probing the origins of particle acceleration on our nearest star

Localization of the Gamma-Ray Emission Region in the 1 September 2014 Behind-the-Limb Solar Flare According to the Fermi/LAT Data

Contact Info

Product

Resources

About