Detection of Quasi-Periodic Pulsations in Solar EUV Time Series

Dominique, Marie; Zhukov, A. N.; Dolla, L.; Inglis, Andrew; Lapenta, G.

doi:10.1007/s11207-018-1281-x

Cited by 43 publications

(34 citation statements)

References 34 publications

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“…No correlations were found with the active region area, magnetic bipole separation distance at the solar surface, or average magnetic field strength. Likewise, no dependence of the QPP period on the flare longitude or the flare class was revealed [9]. Analysis of QPP in the white light emission of stellar flares showed no correlation between the QPP period and the stellar temperatures, radii, rotation periods and surface gravity, and the flare energy [12].…”

Section: Introductionmentioning

confidence: 92%

“…Because of this, a number of recent studies avoided the problem of disentangling the flare trend and red noise by not detrending at all (e.g., [9,10,35]). However the flare trend does have a significant impact on the shape of flare power spectra (e.g., [32]), and as such can make QPP signals much more difficult to detect [35].…”

Section: The Trendmentioning

confidence: 99%

“…Recent commissioning of the new generation of space-borne and ground-based instruments that provide an almost uninterrupted monitoring of the Sun, allowed for statistical studies of QPP. It was established that QPP are a statistically significant feature of solar flares in both non-thermal [7] and thermal [8,9] emission. This conclusion excludes the possible occurrence of apparent QPP because of the red noise or the superposition of multiple unrelated flares.…”

Section: Introductionmentioning

confidence: 99%

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Non-stationary quasi-periodic pulsations in solar and stellar flares

Nakariakov

Kolotkov

Kupriyanova

et al. 2018

Plasma Phys. Control. Fusion

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Often the enhanced electromagnetic radiation generated in solar and stellar flares shows a pronounced (quasi)-oscillatory pattern-quasi-periodic pulsations (QPP), with characteristic periods ranging from a fraction of a second to several tens of minutes. We review recent advances in the empirical study of QPP in solar and stellar flares, addressing the intrinsic nonstationarity of the signal, i.e. the variation of its amplitude, period or phase with time. This nonstationarity could form a basis for a classification of QPP, necessary for revealing specific physical mechanisms responsible for their appearance. We could identify two possible classes of QPP, decaying harmonic oscillations, and trains of symmetric triangular pulsations. Apparent similarities between QPP and irregular geomagnetic pulsations Pi offer a promising avenue for the knowledge transfer in both analytical techniques and theory. Attention is also paid to the effect of the flare trend on the detection and analysis of QPP.

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Section: Introductionmentioning

confidence: 92%

Section: The Trendmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Non-stationary quasi-periodic pulsations in solar and stellar flares

Nakariakov

Kolotkov

Kupriyanova

et al. 2018

Plasma Phys. Control. Fusion

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“…Two theories are proposed to explain the origin of QPP in a flare: repetitive magnetic reconnection (McLaughlin et al 2009(McLaughlin et al , 2012Thurgood et al 2017;McLaughlin et al 2018;Dominique et al 2018) and modulation to the flaring site by magnetohydrodynamic (MHD) waves (Nakariakov et al 2006;Reznikova & Shibasaki 2011;Tian et al 2016). Repetitive magnetic reconnection cannot be observed directly, since coronal magnetic field is extremely difficult to measure with current instrumentation.…”

Section: Introductionmentioning

confidence: 99%

A Compact Source for Quasi-periodic Pulsation in an M-class Solar Flare

Yuan

Feng

Dong

et al. 2019

ApJL

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Quasi-periodic pulsations (QPP) are usually found in the light curves of solar and stellar flares, they carry the features of time characteristics and plasma emission of the flaring core, and could be used to diagnose the coronas of the Sun and remote stars. In this study, we combined the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory and the Nobeyama Radioheliograph (NoRH) to observe an M7.7 class flare occurred at active region 11520 on 19 July 2012. A QPP was detected both in the AIA 131Å bandpass and the NoRH 17 GHz channel, it had a period of about four minutes. In the spatial distribution of Fourier power, we found that this QPP originated from a compact source and that it overlapped with the X-ray source above the loop top. The plasma emission intensities in the AIA 131Å bandpass were highly correlated within this region. The source region is further segmented into stripes that oscillated with distinctive phases. Evidence in this event suggests that this QPP was likely to be generated by intermittent energy injection into the reconnection region.

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“…КПП присутствуют в излучении всего электромагнитного спектра, от радиоволн до гамма-лучей Nakajima et al, 1983;Kupriyanova et al, 2010;Dolla et al, 2012;Simões et al, 2015;Inglis et al, 2016]. Анализируя свойства сигнала в разных диапазонах, а именно его амплитудные, частотные и фазовые характеристики, мы можем строить предположения относительно природы КПП [McLaughlin et al, 2018;Van Doorsselaere et al, 2016;Nakariakov, Melnikov, 2009] (см.…”

Section: статистические свойства кппunclassified

Quasi-periodic pulsations in solar and stellar flares. Review

Kupriyanova

Kolotkov

Nakariakov

et al. 2020

Solnechno-Zemnaya Fizika

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This paper provides an overview of the state-of-the-art studies of oscillatory processes in solar and stellar flares, based on modern observational data from ground-based and space-borne instruments with high temporal, spatial, and spectral resolution in different electro-magnetic spectrum ranges. We examine the mechanisms that generate flare emission and its quasi-periodic modulation. We discuss similarities and differences between solar and stellar flares, and address associated problems of superflares on the Sun and space weather problems. Quasi-periodic pulsations (QPPs) of flare radiation are shown to be an effective tool for diagnosing both the flare processes themselves and the parameters of flare plasma and accelerated particles. We consider types of QPPs, their statistical properties, and methods of analysis, taking into account the non-stationarity of the QPPs’ parameters. We review the proposed mechanisms of QPPs and address open questions.

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Detection of Quasi-Periodic Pulsations in Solar EUV Time Series

Cited by 43 publications

References 34 publications

Non-stationary quasi-periodic pulsations in solar and stellar flares

Non-stationary quasi-periodic pulsations in solar and stellar flares

A Compact Source for Quasi-periodic Pulsation in an M-class Solar Flare

Quasi-periodic pulsations in solar and stellar flares. Review

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