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An HMI LOS magnetogram overlaid with magnetic field lines (pink) extrapolated by using the PFSS model (Schrijver & De Rosa 2003), in which the black and white patches are the regions of negative and positive magnetic polarities, respectively. The dashed blue and green boxes show the FOVs of the panels in Figure 1 and Figure 2, respectively. The green and blue dashed curves mark the position of the QFP wave trains at 03:38:11 UT and 03:47:35 UT in the AIA 171Å171Å images, respectively.
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Using high temporal and high spatial resolution observations taken by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, we present the detailed observational analysis of a high quality quasi-periodic fast- propagating (QFP) magnetosonic wave that was associated with the eruption of a magnetic flux rope and a GOES C5.0 flare....
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... Generally, the most likely relevant driven mechanisms are the energy release in the magnetic reconnections process Shen & Liu 2012;Yuan et al. 2013) and the dispersive evolution (Roberts et al. 1983;Pascoe et al. 2013Pascoe et al. , 2017Nisticò et al. 2014;Shen et al. 2018b). Liu et al. (2011) first reported the association between the flare pulsation detected in hard X-ray by RHESSI and the narrow QFP wave trains' periodicities: the narrow QFP wave trains exhibit a close physical relationship with the accompanying flares, always sharing similar periods and having a close temporal and spatial association (Shen & Liu 2012;Shen et al. 2013bShen et al. , 2018a. In some instances, multiple narrow wave trains with different properties are excited one after another, and each wave train is accompanied by an energy burst (Yuan et al. 2013;Miao et al. 2020;Zhou et al. 2022c), suggesting a strong connection between the flares and the narrow QFP wave trains. ...
This paper presents three distinct wave trains that occurred on 2023 April 21: a broad quasiperiodic fast-propagating (QFP) wave train and bidirectional narrow QFP wave trains. The broad QFP wave train expands outward in a circular wave front, while bidirectional narrow QFP wave trains propagate in the northward and southward directions, respectively. The concurrent presence of the wave trains offers a remarkable opportunity to investigate their respective triggering mechanisms. Measurement shows that the speed of the broad QFP wave train is in the range of 300–1100 km s ⁻¹ in different propagating directions. There is a significant difference in the speed of the bidirectional narrow QFP wave trains: the southward propagation achieves 1400 km s ⁻¹ , while the northward propagation only reaches about 550 km s ⁻¹ accompanied by a deceleration of about 1–2 km s ⁻² . Using the wavelet analysis, we find that the periodicity of the propagating wave trains in the southward and northward directions closely matches the quasiperiodic pulsations exhibited by the flares. Based on these results, the narrow QFP wave trains were most likely excited by the intermittent energy release in the accompanying flare. In contrast, the broad QFP wave train had a tight relationship with the erupting filament, probably attributed to the unwinding motion of the erupting filament, or the leakage of the fast sausage wave train inside the filament body.
... Over the past decade, several observations have shown a close relationship between the QFP wave train and their accompanying flares Shen & Liu 2012c;Yuan et al. 2013;Kumar et al. 2017;Shen et al. 2018bShen et al. , 2018c. These researchers found that the initial position of the QFP wave train is usually a few megameters from the flare core, and the periods of the QFP waves are usually partially or completely similar to the periods of the related flare. ...
We present the observations of multimode kink waves and a narrow quasiperiodic fast-propagating (QFP) wave train in association with a jet on 2011 December 11. The jet impinged on a loop, which excited a propagating kink mode transitioning into a standing kink mode and also excited a QFP wave train away from the jet. Motion magnification is used to fit the higher harmonic standing wave oscillation profile with three periods at three different spatial locations. The periods have the ratio 6:3:2. The ratio of the fundamental mode to the second harmonic of the standing wave is about 1.95, suggesting that the magnetic field strength variation effect is strong enough to cancel out the density stratification. The differential emission measure is used to estimate the loop’s plasma property at these three points, and it found the density and the temperature are roughly constant. The magnetic field strength, B = 51 ± 16 G, is derived by the coronal seismology using the fundamental kink mode. It is striking to find that the the ratio of the second harmonic to the third harmonic of the kink wave coincides with that of the periods of the QFP wave train, and the ratio of periods is about 1.5 in both cases. We propose that the excitation of the high-order harmonics and the QFP wave train could be the nonlinear response of the steep density-gradient plasma interacting with electromagnetic field in the southwest foot region. This region, like a resonator, might play an important role in energy reservoir capture and act as a frequency filter to generate propagating waves of particular frequencies.
... Observational signatures of chromospheric jets by periodic reconnection events have also been reported in simulations by Heggland et al. (2009), although, the periodicity was attributed to the continuous driving rather than being inherent to the system. Oscillatory reconnection has also been considered as a possible mechanism behind the creation of an observed quasiperiodic fast-propagating (QFP) magnetosonic wave from the eruption of a magnetic flux rope (Shen et al. 2018), as well as behind the formation and disappearance of a small-scale magnetic flux rope consisting of new loops formed by the reconnection events (Xue et al. 2019). Zhang et al. (2014) reported oscillatory (or reciprocatory) magnetic reconnection in observations of coronal bright points (CBPs), while reversals of an elongated current sheet in a recent numerical 2D CBP model have been attributed to oscillatory reconnection (Nobrega-Siverio & Moreno-Insertis 2022). ...
... However, the derived relation can be a useful plasma diagnostic tool in coronal conditions, and needs to be tested further against observational periodic signals, which could be attributed to oscillatory reconnection. Such periodic signals in the solar atmosphere include, but are not limited to, QPPs of solar (e.g., Kupriyanova et al. 2016) and stellar flares (e.g., Broomhall et al. 2019), quasi-periodic chromospheric (e.g., De Pontieu et al. 2011) and coronal jets (e.g., Hong et al. 2019;Mandal et al. 2022), QFP magnetosonic wave from the eruption of a magnetic flux rope (e.g., Shen et al. 2018), and periodicities correlated with Type III radio bursts (Cattell et al. 2021). A detailed discussion of the different phenomena attributed to oscillatory reconnection has already been presented in Section 1. ...
Oscillatory reconnection is a relaxation process in magnetized plasma, with an inherent periodicity that is exclusively dependent on the properties of the background plasma. This study focuses on the seismological prospects of oscillatory reconnection in the solar corona. We perform three sets of parameter studies (for characteristic coronal values of the background magnetic field, density, and temperature) using the PLUTO code to solve the fully compressive, resistive MHD equations for a 2D magnetic X-point. From each parameter study, we derive the period of the oscillatory reconnection. We find that this period is inversely proportional to the characteristic strength of the background magnetic field and the square root of the initial plasma temperature, while following a square root dependency upon the equilibrium plasma density. These results reveal an inverse proportionality between the magnitude of the Alfvén speed and the period, as well as the background speed of sound and the period. Furthermore, we note that the addition of anisotropic thermal conduction only leads to a small increase in the mean value for the period. Finally, we establish an empirical formula that gives the value for the period in relation to the background magnetic field, density, and temperature. This gives us a quantified relation for oscillatory reconnection, to be used as a plasma diagnostic in the solar corona, opening up the possibility of using oscillatory reconnection for coronal seismology.
... Observational signatures of chromospheric jets by periodic reconnection events were also reported in simulations by Heggland et al. (2009), although, the periodicity was attributed to the continuous driving rather than being inherent to the system. Oscillatory reconnection has also been considered as a possible mechanism behind with the creation of an observed quasi-periodic fastpropagating (QFP) magnetosonic wave from the eruption of a magnetic flux rope (Shen et al. 2018), as well as behind the formation and disappearance of a small scale magnetic flux rope consisting of new loops formed by the reconnection events (Xue et al. 2019). Zhang et al. (2014) have reported oscillatory (or reciprocatory) magnetic reconnection in observations of Coronal Bright Points (CBPs), while reversals of an elongated current sheet in a recent numerical 2D CBP model has been attributed to oscillatory reconnection (Nóbrega-Siverio & Moreno-Insertis 2022). ...
... Hong et al. 2019;Mandal et al. 2022), quasi-periodic fast-propagating (QFP) magnetosonic wave from the eruption of a magnetic flux rope (e.g. Shen et al. 2018) and periodicities correlated with Type III radio bursts (Cattell et al. 2021). A detailed discussion of the different phenomena attributed to oscillatory reconnection has already been presented in the Section 1. ...
Oscillatory reconnection is a relaxation process in magnetised plasma, with an inherent periodicity that is exclusively dependent on the properties of the background plasma. This study focuses on the seismological prospects of oscillatory reconnection in the solar corona. We perform three sets of parameter studies (for characteristic coronal values of the background magnetic field, density and temperature) using the PLUTO code to solve the fully compressive, resistive MHD equations for a 2D magnetic X-point. From each parameter study, we derive the period of the oscillatory reconnection. We find that this period is inversely proportional to the characteristic strength of the background magnetic field and the square root of the initial plasma temperature, while following a square root dependency upon the equilibrium plasma density. These results reveal an inverse proportionality between the magnitude of the Alfv\'en speed and the period, as well as the background sound speed and the period. Furthermore, we note that the addition of anisotropic thermal conduction only leads to a small increase in the mean value for the period. Finally, we establish an empirical formula that gives the value for the period in relation to the background magnetic field, density and temperature. This gives us a quantified relation for oscillatory reconnection, to be used as a plasma diagnostic in the solar corona, opening up the possibility of using oscillatory reconnection for coronal seismology.
... Therefore, we speculate that these wave trains should be excited by the intermittent energy releases rather than the dispersive mechanism. In addition, the leakage of pressure-driven p-mode oscillation from the photosphere and chromosphere into the corona (Shen & Liu 2012b), slowmode magnetosonic waves leaking from the 3 minute chromospheric sunspot oscillations (Sych et al. 2009), the magnetic reconnection between the loop system (Kumar et al. 2017;Li et al. 2018b;Shen et al. 2022a), the eruption of the magnetic flux rope (Shen et al. 2018b;Wang et al. 2020), and the successive stretching of magnetic field structures (Shen et al. 2018d;Sun et al. 2022), as well as the jet (Shen et al. 2018a;Duan et al. 2022), are all thought to be candidate drivers of QFP wave trains. ...
About the driven mechanisms of the quasiperiodic fast-propagating (QFP) wave trains, there exist two dominant competing physical explanations: they are associated with the flaring energy release or attributed to the waveguide dispersion. Employing Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å images, we investigated a series of QFP wave trains composed of multiple wave fronts propagating along a loop system during the accompanying flare on 2011 November 11. The wave trains showed a high correlation in start times with the energy release of the accompanying flare. Measurements show that the wave trains’ phase speed is almost consistent with its group speed with a value of about 1000 km s ⁻¹ , indicating that the wave trains should not be considered dispersed waves. The period of the wave trains was the same as that of the oscillatory signal in X-ray emissions released by the flare. Thus we propose that the QFP wave trains were most likely triggered by the flare rather than by dispersion. We investigated the seismological application with the QFP waves and then obtained that the magnetic field strength of the waveguide was about 10 G. Meanwhile, we also estimated that the energy flux of the wave trains was about 1.2 × 10 ⁵ erg cm ⁻² s ⁻¹ .
... Therefore, we speculate that these wave trains should be excited by the intermittent energy releases rather than the dispersive mechanism. In addition, the leakage of pressure-driven p−modes oscillation from the photosphere and chromosphere into the corona (Shen & Liu 2012b), slow-mode magnetosonic waves leaking from the 3-minute chromospheric sunspot oscillations (Sych et al. 2009), the magnetic reconnection between the loop system (Kumar et al. 2017;Li et al. 2018b;Shen et al. 2022a), the eruption of the magnetic flux rope (Shen et al. 2018b;Wang et al. 2020), the successive stretching of magnetic field structrues (Shen et al. 2018d;Sun et al. 2022), as well as the jet (Shen et al. 2018a;Duan et al. 2022) are both thought to be candidate drivers of QFP wave trains. ...
About the driven mechanisms of the quasi-periodic fast-propagating (QFP) wave trains, there exist two dominant competing physical explanations: associated with the flaring energy release or attributed to the waveguide dispersion. Employing Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) 171 Å images , we investigated a series of QFP wave trains composed of multiple wavefronts propagating along a loop system during the accompanying flare on 2011 November 11. The wave trains showed a high correlation in start time with the energy release of the accompanying flare. Measurements show that the wave trains' phase speed is almost consistent with its group speed with a value of about 1000 km s −1 , indicating that the wave trains should not be dispersed waves. The period of the wave trains was the same as that of the oscillatory signal in X-ray emissions released by the flare. Thus we propose that the QFP wave trains were most likely triggered by the flare rather than by dispersion. We investigated the seismological application with the QFP waves and then obtained that the magnetic field strength of the waveguide was about 10 Gauss. Meanwhile, we also estimated that the energy flux of the wave trains was about 1.2 × 10 5 erg · cm −2 s −1 .
... The observed QFP waves often consist of multiple concentric and coherent wavefronts, termed as 'QFP wave trains,' and they are produced successively within periods of dozens of seconds or a few minutes near the epicenter of the accompanying flares (Shen et al., 2022b,a). Sometimes, the quasi-periods of QFP wave trains are quite similar to those of associated flare QPPs, implying that the two different phenomena might manifest the two different aspects of the same physical process, that is, the pulsed energy release via repeating magnetic reconnection Shen et al., 2013Shen et al., , 2018bKolotkov et al., 2018;Zhou et al., 2022). On the other hand, some quasi-periods of QFP wave trains are completely unassociated with those of flare QPPs, indicating that the periodicity of QFP wave trains is diverse and could not be associated with flare QPPs (Shen et al., 2018c(Shen et al., , 2019. ...
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 × 10 ¹⁰ 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.
... The observed QFP waves often consist of multiple concentric and coherent wavefronts, termed as 'QFP wave trains', and they are produced successively within periods of dozens of seconds or a few minutes near the epicenter of the accompanying flares (Shen et al., 2022b,a). Sometimes, the quasi-periods of QFP wave trains are quite similar to those of associated flare QPPs, implying that the two different phenomena might manifest the two different aspects of the same physical process, i.e., the pulsed energy release via repeating magnetic reconnection Shen et al., 2013Shen et al., , 2018bKolotkov et al., 2018;Zhou et al., 2022). On the other hand, some quasi-periods of QFP wave trains are completely unassociated with those of flares QPPs, indicating that the periodicity of QFP wave trains is diverse and could not be associated with flare QPPs (Shen et al., 2018c(Shen et al., , 2019. ...
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 paper, we investigated non-stationary QPPs associated with recurrent jets during an M1.2 flare on 2022 July 14. A quasi-period of about 45$\pm$10 s, determined by the wavelet transform technique, is simultaneously identified at wavelengths of soft/hard X-ray and microwave emissions, which are recorded by the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor, Fermi, and the Nobeyama Radio Polarimeters, respectively. A group of recurrent jets with an intermittent cadence of about 45$\pm$10 s are found in Atmospheric Imaging Assembly (AIA) image series at 304 {\AA}, but they are 180-s earlier than the flare QPP. All observational facts suggest that the flare QPP could be excited by recurrent jets, and they should be associated with nonthermal electrons that are periodically accelerated by a repeated energy release process, like repetitive magnetic reconnection. Moreover, the same quasi-period is discovered at double footpoints connected by a hot flare loop in AIA 94 {\AA}, and the phase speed is measured to 1420 km/s. Based on the differential emission measure, the average temperatures, number densities, and magnetic field strengths at the loop top and footpoint are estimated to 7.7/6.7 MK, 7.5/3.6*10^{10} 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.
... Alongside QPPs, oscillatory reconnection can also be associated with quasi-periodic flows associated with spicules (e.g. De Pontieu & McIntosh 2010;De Pontieu et al. 2011;Samanta et al. 2019;Yurchyshyn et al. 2020), as well as with observed periodicities in jets (Hong et al. 2019) and in the formation, disappearance, and eruption of magnetic flux ropes (Shen et al. 2018;Xue et al. 2019). McLaughlin et al. (2012b) were able to reproduce such observed periodicities through oscillatory reconnection in a 2D flux emergence model. ...
Oscillatory reconnection can manifest through the interaction between the ubiquitous MHD waves and omnipresent null points in the solar atmosphere and is characterized by an inherent periodicity. In the current study, we focus on the relationship between the period of oscillatory reconnection and the strength of the wave pulse initially perturbing the null point, in a hot coronal plasma. We use the PLUTO code to solve the fully compressive, resistive MHD equations for a 2D magnetic X-point. Using wave pulses with a wide range of amplitudes, we perform a parameter study to obtain values for the period, considering the presence and absence of anisotropic thermal conduction separately. In both cases, we find that the resulting period is independent of the strength of the initial perturbation. The addition of anisotropic thermal conduction only leads to an increase in the mean value for the period, in agreement with our previous study. We also consider a different type of initial driver and we obtain an oscillation period matching the independent trend previously mentioned. Thus, we report for the first time on the independence between the type and strength of the initializing wave pulse and the resulting period of oscillatory reconnection in a hot coronal plasma. This makes oscillatory reconnection a promising mechanism to be used within the context of coronal seismology.
... Alongside QPPs, oscillatory reconnection can also be associated with quasi-periodic flows associated with spicules (e.g., De Pontieu & McIntosh 2010;De Pontieu et al. 2011;Samanta et al. 2019;Yurchyshyn et al. 2020), as well as with observed periodicities in jets (Hong et al. 2019) and in the formation, disappearance, and eruption of magnetic flux ropes (Shen et al. 2018;Xue et al. 2019). McLaughlin et al. (2012b) were able to reproduce such observed periodicities through oscillatory reconnection in a 2D flux emergence model. ...
Oscillatory reconnection can manifest through the interaction between the ubiquitous MHD waves and omnipresent null points in the solar atmosphere and is characterized by an inherent periodicity. In the current study, we focus on the relationship between the period of oscillatory reconnection and the strength of the wave pulse initially perturbing the null point, in a hot coronal plasma. We use the PLUTO code to solve the fully compressive, resistive MHD equations for a 2D magnetic X-point. Using wave pulses with a wide range of amplitudes, we perform a parameter study to obtain values for the period, considering the presence and absence of anisotropic thermal conduction separately. In both cases, we find that the resulting period is independent of the strength of the initial perturbation. The addition of anisotropic thermal conduction only leads to an increase in the mean value for the period, in agreement with our previous study. We also consider a different type of initial driver and we obtain an oscillation period matching the independent trend previously mentioned. Thus, we report for the first time on the independence between the type and strength of the initializing wave pulse and the resulting period of oscillatory reconnection in a hot coronal plasma. This makes oscillatory reconnection a promising mechanism to be used within the context of coronal seismology.
