Flare quasi-periodic pulsation associated with recurrent jets

Liu, Dong; Shi, Fanpeng; Zhao, H. S.; Xiong, S. L.; Song, Liming; Peng, W. X.; Li, Xinqiao; Chen, Wei; Ning, Zongjun

doi:10.3389/fspas.2022.1032099

Cited by 16 publications

(5 citation statements)

References 133 publications

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“…The third type may be caused by changes in the magnetic field configuration during the first reconnection, which affects the subsequent eruption. Most of these jets also show repeated blobs, which could arise from the quasi-periodic reconnection that has been observed in some solar flares (Shi et al 2022a,b;Li et al 2022). By combining the Solar Orbiter/EUI observation with a simultaneous observation from SDO/AIA, the jets' physical parameters and energies were measured.…”

Section: Discussionmentioning

confidence: 99%

Energy estimation of small-scale jets from the quiet-Sun region

Shi,

Li,

Ning

et al. 2024

A&A

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Context. Solar jets play a role in coronal heating and the supply of solar wind. Aims. In this study, we calculate the energies of 23 small-scale jets emerging from a quiet-Sun region in order to investigate their contributions to coronal heating. Methods. We used data from the High-Resolution Imager (HRI) of the Extreme Ultraviolet Imager (EUI) on board the Solar Orbiter. Small-scale jets were observed by the HRIEUV 174 Å passband in the high cadence of 6 s. These events were identified by the time–distance stacks along the trajectories of jets. Using the simultaneous observation from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO), we also performed a differential emission measure (DEM) analysis on these small-scale jets to obtain the physical parameters of plasma, which enabled us to estimate the kinetic and thermal energies of the jets. Results. We find that most of the jets exhibit common unidirectional or bidirectional motions, while some show more complex behaviors; namely, a mixture of unidirection and bidirection. A majority of jets also present repeated eruption blobs (plasmoids), which may be signatures of the quasi-periodic magnetic reconnection that has been observed in solar flares. The inverted Y-shaped structure can be recognized in several jets. These small-scale jets typically have a width of ∼0.3 Mm, a temperature of ∼1.7 MK, an electron number density of ≳109 cm−3, with speeds in a wide range from ∼20–170 km s−1. Most of these jets have an energy of 1023–1024 erg, which is marginally smaller than the energy of typical nanoflares. The thermal energy fluxes of 23 jets are estimated to be (0.74–2.96)×105 erg cm−2 s−1, which is almost on the same order of magnitude as the energy flow required to heat the quiet-Sun corona, although the kinetic energy fluxes vary over a wide range because of their strong dependence on velocity. Furthermore, the frequency distribution of thermal energy and kinetic energy both follow the power-law distribution N(E)∝E−α. Conclusions. Our observations suggest that although these jets cannot provide sufficient energy to heat the whole quiet-Sun coronal region, they are likely to account for a significant portion of the energy demand in the local regions where the jets occur.

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Section: Discussionmentioning

confidence: 99%

Energy estimation of small-scale jets from the quiet-Sun region

Shi,

Li,

Ning

et al. 2024

A&A

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“…Mishra et al [46] found a period of about 3 min in a blowout jet mainly composed of cool material and the research strongly supports the fact that multiple magnetic reconnection triggers QPPs in the blowout jet. Li et al [47] 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.…”

Section: Discussionmentioning

confidence: 99%

Quasi-Periodic Pulsations in an M-Class Solar Flare

Ning

et al. 2023

Universe

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We have studied the quasi-periodic pulsations (QPPs) of the M2.3 flare that occurred in the active region NOAA 12172 on 23 September 2014. Through the fast Fourier transform (FFT) method, we decompose the flare light curves into fast- and slowly-varying components, and the cut-off threshold is 100 s. We find that the QPPs have a period of 40 s at soft X-ray (SXR), hard X-ray (HXR), radio and ultraviolet (UV). Based on the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO), we find that the QPPs take place at the same time interval as the flare ribbon separation, and that the QPPs seem to originate from the flare ribbons. Our observations tend to support the mechanism of the periodic nonthermal electron injection during the flare eruption.

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“…QPPs have been identified with timescales ranging from seconds to minutes (e.g. Zhao et al 2023;Kou et al 2022;Lörinčík et al 2022;Li et al 2022;Zimovets et al 2022), with few studies reporting subsecond QPPs (e.g. Knuth & Glesener 2020;Qiu et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Localising pulsations in the hard X-ray and microwave emission of an X-class flare

Collier,

Hayes,

et al. 2024

A&A

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The aim of this work is to identify the mechanism driving pulsations in hard X-ray (HXR) and microwave emission during solar flares. Using combined HXR and microwave observations from Solar Orbiter/STIX and EOVSA, we investigate an X1.3 GOES class flare, 2022-03-30T17:21:00, which displays pulsations on timescales evolving from $ 7$ s in the impulsive phase to $ s later in the flare. We analysed the temporal, spatial, and spectral evolution of the HXR and microwave pulsations during the impulsive phase of the flare. We reconstructed images for individual peaks in the impulsive phase and performed spectral fitting at high cadence throughout the first phase of pulsations. Our imaging analysis demonstrates that the HXR and microwave emission originates from multiple sites along the flare ribbons. The brightest sources and the location of the emission change in time. Through HXR spectral analysis, the electron spectral index is found to be anti-correlated with the HXR flux, showing a `soft-hard-soft' spectral index evolution for each pulsation. The timing of the associated filament eruption coincides with the early impulsive phase. Our results indicate that periodic acceleration and/or injection of electrons from multiple sites along the flare arcade is responsible for the pulsations observed in HXR and microwave emission. The evolution of pulsation timescales is likely a result of changes in the 3D magnetic field configuration over time related to the associated filament eruption.

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Flare quasi-periodic pulsation associated with recurrent jets

Cited by 16 publications

References 133 publications

Energy estimation of small-scale jets from the quiet-Sun region

Energy estimation of small-scale jets from the quiet-Sun region

Quasi-Periodic Pulsations in an M-Class Solar Flare

Localising pulsations in the hard X-ray and microwave emission of an X-class flare

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