Persistent Quasi-Periodic Pulsations During a Large X-Class Solar Flare
| Autor: | Brian R. Dennis, Laura A. Hayes, Jack Ireland, Diana E. Morosan, Peter T. Gallagher, Andrew Inglis |
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| Přispěvatelé: | Department of Physics |
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
Sun: flares
010504 meteorology & atmospheric sciences Astrophysics::High Energy Astrophysical Phenomena WAVES Phase (waves) FOS: Physical sciences Plasmoid Astrophysics ACCELERATION ACOUSTIC-OSCILLATIONS 01 natural sciences law.invention law 0103 physical sciences Coronal mass ejection RAY PULSATIONS RHESSI Astrophysics::Solar and Stellar Astrophysics Geostationary Operational Environmental Satellite Sun: oscillations MICROWAVE 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) 0105 earth and related environmental sciences Physics RADIO Solar flare Gamma ray Astronomy and Astrophysics 115 Astronomy Space science gamma rays Amplitude Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Physics::Space Physics EMISSION Sun: X-rays Flare |
| Popis: | Solar flares often display pulsating and oscillatory signatures in the emission, known as quasi-periodic pulsations (QPP). QPP are typically identified during the impulsive phase of flares, yet in some cases, their presence is detected late into the decay phase. Here, we report extensive fine structure QPP that are detected throughout the large X8.2 flare from 2017 September 10. Following the analysis of the thermal pulsations observed in the GOES/XRS and the 131 A channel of SDO/AIA, we find a pulsation period of ~65 s during the impulsive phase followed by lower amplitude QPP with a period of ~150 s in the decay phase, up to three hours after the peak of the flare. We find that during the time of the impulsive QPP, the soft X-ray source observed with RHESSI rapidly rises at a velocity of approximately 17 km/s following the plasmoid/coronal mass ejection (CME) eruption. We interpret these QPP in terms of a manifestation of the reconnection dynamics in the eruptive event. During the long-duration decay phase lasting several hours, extended downward contractions of collapsing loops/plasmoids that reach the top of the flare arcade are observed in EUV. We note that the existence of persistent QPP into the decay phase of this flare are most likely related to these features. The QPP during this phase are discussed in terms of MHD wave modes triggered in the post-flaring loops. Accepted for publication in ApJ - 13 pages, 9 figures, 1 accompanying movie found at -https://tinyurl.com/yykvd8pf |
| Databáze: | OpenAIRE |
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