Persistent Quasi-periodic Pulsations during a Large X-class Solar Flare

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http://hdl.handle.net/10138/303515

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Hayes , L A , Gallagher , P T , Dennis , B R , Ireland , J , Inglis , A & Morosan , D E 2019 , ' Persistent Quasi-periodic Pulsations during a Large X-class Solar Flare ' , Astrophysical Journal , vol. 875 , no. 1 , 33 . https://doi.org/10.3847/1538-4357/ab0ca3

Title: Persistent Quasi-periodic Pulsations during a Large X-class Solar Flare
Author: Hayes, Laura A.; Gallagher, Peter T.; Dennis, Brian R.; Ireland, Jack; Inglis, Andrew; Morosan, Diana E.
Contributor: University of Helsinki, Department of Physics
Date: 2019-04-10
Language: eng
Number of pages: 11
Belongs to series: Astrophysical Journal
ISSN: 0004-637X
URI: http://hdl.handle.net/10138/303515
Abstract: 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 Geostationary Operational Environmental Satellite/X-ray sensor and the 131 angstrom channel of Solar Dynamics Observatory/Atmospheric Imaging Assembly, we find a pulsation period of similar to 65 s during the impulsive phase followed by lower amplitude QPP with a period of similar to 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 the Reuven Ramaty High Energy Solar Spectroscopic Imager rapidly rises at a velocity of approximately 17 km s(-1) following the plasmoid/coronal mass ejection 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 magnetohydrodynamic wave modes triggered in the post-flaring loops.
Subject: Sun: flares
Sun: oscillations
Sun: X-rays
gamma rays
ACOUSTIC-OSCILLATIONS
RAY PULSATIONS
EMISSION
RADIO
ACCELERATION
MICROWAVE
RHESSI
WAVES
115 Astronomy, Space science
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