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Persistent Quasi-Periodic Pulsations During a Large X-Class Solar Flare View all abstracts by submitter

Laura A. Hayes   Submitted: 2019-03-05 06:46

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 Å 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-1 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.

Authors: Laura A. Hayes, Peter T. Gallagher, Brian R. Dennis, Jack Ireland, Andrew Inglis, and Diana E. Morosan
Projects: None

Publication Status: Accepted ApJ
Last Modified: 2019-03-05 12:47
Go to main E-Print page  Properties of slow magnetoacoustic oscillations of solar coronal loops by multi-instrumental observations  Magnetic helicity and fluxes in an inhomogeneous alpha squared dynamo  Edit Entry  Download Preprint  Delete Entry 

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