Common Origin of Quasi-Periodic Pulsations in Microwave and Decimetric Solar Radio Bursts

Kashapova, L. K.; Kolotkov, Dmitrii Y.; Kupriyanova, E. G.; Kudriavtseva, Anastasiia; Tan, Cuiyan; Reid, Hamish

doi:10.1007/s11207-021-01934-x

Cited by 10 publications

(7 citation statements)

References 59 publications

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“…The phenomenon of quasi-periodic bursts can be attributed to many physical processes like periodic reconnections, loop oscillations, etc. (Nakariakov & Melnikov 2009;Kashapova et al 2021). In meter waves, several quasi-periodic oscillations during type-I (Mohan 2021b; Mondal & Oberoi 2021) and type-III bursts (Mohan et al 2019) have been reported.…”

Section: Quasi-periodic Burstsmentioning

confidence: 99%

Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona

Sharma

Oberoi

Battaglia

et al. 2022

ApJ

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A ubiquitous presence of weak energy releases is one of the most promising hypotheses to explain coronal heating, referred to as the nanoflare hypothesis. The accelerated electrons associated with such weak heating events are also expected to give rise to coherent impulsive emission via plasma instabilities in the meterwave radio band, making this a promising spectral window to look for their presence. Recently Mondal et al. reported the presence of weak and impulsive emissions from quiet Sun regions which seem to meet the requirements of being radio counterparts of the hypothesized nanoflares. Detection of such low-contrast weak emission from the quiet Sun is challenging and, given their implications, it is important to confirm their presence. In this work, using data from the Murchison Widefield Array, we explore the use of an independent robust approach for their detection by separating the dominant, slowly varying component of emission from the weak impulsive one in the visibility domain. We detect milli-Solar Flux Unit-level bursts taking place all over the Sun and characterize their brightness temperatures, distributions, morphologies, durations, and associations with features seen in extreme-UV images. We also attempt to constrain the energies of the nonthermal particles using inputs from the FORWARD coronal model along with some reasonable assumptions, and find them to lie in the subpico flare (∼1019–1021 erg) range. In the process, we also discover perhaps the weakest type III radio burst and another that shows clear signatures of the weakest quasi-periodic pulsations.

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Section: Quasi-periodic Burstsmentioning

confidence: 99%

Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona

Sharma

Oberoi

Battaglia

et al. 2022

ApJ

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“…Because it is unnecessary to discuss the periodic behavior if there are only one or two peaks, which might be just a coincidence, for instance, the similar time interval between successive peaks occurred by chance (Nakariakov et al 2019;Li 2022a). The flare-related QPPs have been detected almost in the entire solar spectrum, i.e., radio/microwaves, white lights, Hα, ultraviolet/extreme ultraviolet (UV/EUV), Lyα, soft/hard X-rays (SXR/HXR), and γrays (e.g., Nakariakov et al 2010;Li et al 2020aLi et al , 2020bClarke et al 2021;Hong et al 2021;Kashapova et al 2021;Zhao et al 2021;Karlický et al 2022;Li 2022b;Shi et al 2022). The observed quasi-periods vary from subseconds to several tens of minutes (Melnikov et al 2005;Ning 2017;Hayes et al 2020;Karlický & Yasnov 2021;Zimovets et al 2021a;Howard & MacGregor 2022;Ning et al 2022;Shen et al 2022;Zhou et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Quasi-periodic Accelerations of Energetic Particles during a Solar Flare

Chen

2022

ApJL

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We report the observation of nonstationary quasi-periodic pulsations (QPPs) in high-energy particles during the impulsive phase of an X4.8 flare on 2002 July 23 (SOL2002-07-23T00:35). The X4.8 flare was simultaneously measured by the Reuven Ramaty High Energy Solar Spectroscopic Imager, Nobeyama Radio Polarimeters, and Nobeyama Radioheliograph. The quasi-period of ∼50 ± 15 s, determined by the wavelet transform, is detected in the γ-ray line emission. Using the same method, a quasi-period of ∼90 ± 20 s is found in the γ-ray continuum, hard X-ray (HXR), and radio emissions during almost the same time. Our observations suggest that the flare QPPs should be associated with energetic ions and nonthermal electrons that are quasi-periodically accelerated by the repetitive magnetic reconnection. The different quasi-periods between the γ-ray line and continuum/HXR/radio emissions indicate an apparent difference in acceleration or propagation between energetic ions and nonthermal electrons of this solar flare.

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“…They are frequently identified as a series of repetitive but irregular pulsations with anharmonic and symmetric triangular shapes, referring to non-stationary QPPs (e.g., Nakariakov et al, 2019). The observation of QPPs has been reported in flare time series over a broad range of wavelengths, ranging from radio/microwave emissions through ultraviolet (UV) and white light wavelengths to soft and hard X-rays (SXR/HXR) channels, and even in the γ-ray emission (e.g., Nakariakov et al, 2010a;Tan et al, 2016;Milligan et al, 2017;Li et al, 2017b;Kashapova et al, 2021;Kolotkov et al, 2021;Lu et al, 2021;Doyle et al, 2022;Smith et al, 2022;Zhang et al, 2022a). Generally, a typical QPP should be at least three successive and complete pulsations.…”

Section: Introductionmentioning

confidence: 99%

“…The flare QPPs with long periods in the order of seconds and minutes, which could detect in almost all wavelengths, are frequently interpreted in terms of magnetohydrodynamic (MHD) waves in slow modes (e.g., Wang et al, 2021), kink modes (e.g., Nakariakov et al, 2021), and sausage modes (e.g., Li et al, 2020a). In such case, the flare QPPs with periods larger than 1 minute could be associated with slow sausage waves (Sadeghi and Karami, 2019;Gao et al, 2021), global kink waves (Duckenfield et al, 2019;Gao et al, 2022), and slow magnetoacoustic waves (Wang, 2011;Ofman et al, 2012;Yuan et al, 2015;Prasad et al, 2022); while those with periods in the order of seconds are often explained as fast sausage or kink waves (Inglis and Nakariakov, 2009;Guo et al, 2021;Kashapova et al, 2021), depending on whether the plasma loop can be compressible or incompressible (Yuan and Van Doorsselaere, 2016;Nakariakov and Kolotkov, 2020). Those long-period QPPs might be also associated with the repetitive magnetic reconnection (Thurgood et al, 2019;Karampelas et al, 2022).…”

Section: Introductionmentioning

confidence: 99%

Flare quasi-periodic pulsation associated with recurrent jets

Liu

Shi

Zhao

et al. 2022

Front. Astron. Space Sci.

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Quasi-periodic pulsations (QPPs), which carry time features and plasma characteristics of flare emissions, are frequently observed in light curves of solar/stellar flares. In this study, we investigated non-stationary QPPs associated with recurrent jets during an M1.2 flare on 2022 July 14. A quasi-period of ∼45±10 s, determined by the wavelet transform technique, is simultaneously identified at wavelengths of soft/hard X-ray and microwave emissions, which are recorded by the Gravitational Wave High-Energy Electromagnetic Counterpart All-sky Monitor, Fermi and the Nobeyama Radio Polarimeters, respectively. A group of recurrent jets with an intermittent cadence of about 45 ± 10 s are found in the Atmospheric Imaging Assembly (AIA) image series at 304 Å, but they are 180 s earlier than the flare QPP. All observational facts suggest that the flare QPPs could be excited by recurrent jets, and they should be associated with non-thermal electrons that are periodically accelerated by a repeated energy release process, such as repetitive magnetic reconnection. Moreover, the same quasi-period is discovered at double footpoints connected by a hot flare loop in AIA 94 Å, and the phase speed is measured to be ∼1,420 km s−1. Based on the differential emission measure, the average temperatures, number densities, and magnetic field strengths at the loop top and footpoint are estimated to be ∼7.7/6.7 MK, ∼7.5/3.6 × 1010 cm−3, and ∼143/99 G, respectively. Our measurements indicate that the 45-s QPP is probably modulated by the kink-mode wave of the flare loop.

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Common Origin of Quasi-Periodic Pulsations in Microwave and Decimetric Solar Radio Bursts

Abstract: How to cite:Please refer to published version for the most recent bibliographic citation information.

Cited by 10 publications

References 59 publications

Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona

Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona

Quasi-periodic Accelerations of Energetic Particles during a Solar Flare

Flare quasi-periodic pulsation associated with recurrent jets

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