The Trigger Mechanism of Recurrent Solar Active Region Jets Revealed by the Magnetic Properties of a Coronal Geyser Site

Paraschiv, Alin Rǎzvan; Donea, Alina-Catalina; Leka, K. D.

doi:10.3847/1538-4357/ab7246

Cited by 12 publications

(18 citation statements)

References 57 publications

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“…8 is intermittent, rather than continuous, as indicated by the quasi-periodic jets. What determines the ∼68.9 min quasi-period of the reconnection (hence the jets) remains an interesting question that needs to be explored (Chen et al 2015;Cheung et al 2015;Paraschiv et al 2020).…”

Section: How Filament Decayless Oscillations Are Maintainedmentioning

confidence: 99%

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Guo

Zhang

et al. 2022

A&A

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Context. As a ubiquitous phenomenon, large-amplitude longitudinal filament oscillations usually decay in 1–4 periods. Recently, we observed a decayless case of such oscillations in the corona. Aims. We try to understand the physical process that maintains the decayless oscillation of the filament. Methods. Multiwavelength imaging observations and magnetograms were collected to study the dynamics of the filament oscillation and its associated phenomena. To explain the decayless oscillations, we also performed one-dimensional hydrodynamic numerical simulations using the code MPI-AMRVAC. Results. In observations, the filament oscillates without decay with a period of 36.4 ± 0.3 min for almost 4 h before eruption. During oscillations, four quasi-periodic jets emanate from a magnetic cancellation site near the filament. The time interval between neighboring jets is ∼68.9 ± 1.0 min. Numerical simulations constrained by the observations reproduced the decayless longitudinal oscillations. However, it is surprising to find that the period of the decayless oscillations is not consistent with the pendulum model. Conclusions. We propose that the decayless longitudinal oscillations of the filament are maintained by quasi-periodic jets, which is verified by the hydrodynamic simulations. More importantly, it is found that, when it is driven by quasi-periodic jets, the period of the filament longitudinal oscillations also depends on the driving period of the jets, not on the pendulum period alone. With a parameter survey in simulations, we derived a formula by which the pendulum oscillation period can be derived using the observed period of decayless filament oscillations and the driving periods of jets.

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Section: How Filament Decayless Oscillations Are Maintainedmentioning

confidence: 99%

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Guo

Zhang

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…8 is intermittent, rather than continuous, as indicated by the quasi-periodic jets. What determines the ∼68.9 min quasi-period of the reconnection (hence the jets) remains an interesting question noteworthy to be explored (Chen et al 2015;Cheung et al 2015;Paraschiv et al 2020).…”

Section: How Filament Decayless Oscillations Are Maintainedmentioning

confidence: 99%

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Ni,

Guo,

Zhang

et al. 2022

Preprint

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Context. As a ubiquitous phenomenon, large-amplitude longitudinal filament oscillations usually decay in 1-4 periods. Recently, we observed a decayless case of such oscillations in the corona. Aims. We try to understand the physical process that maintains the decayless oscillation of the filament. Methods. Multi-wavelength imaging observations and magnetograms are collected to study the dynamics of the filament oscillation and its associated phenomena. To explain the decayless oscillations, we also perform one-dimensional hydrodynamic numerical simulations using the MPI-AMRVAC code. Results. In observations, the filament oscillates decaylessly with a period of 36.4 ± 0.3 min for almost 4 hours before eruption. During oscillations, four quasi-periodic jets emanate from a magnetic cancellation site near the filament. The time interval between neighboring jets is ∼ 68.9 ± 1.0 min. Numerical simulations constrained by the observations reproduced the decayless longitudinal oscillations. However, it is surprising to find that the period of the decayless oscillations is not consistent with the pendulum model. Conclusions. We propose that the decayless longitudinal oscillations of the filament are maintained by quasi-periodic jets, which is verified by the hydrodynamic simulations. More importantly, it is found that, when driven by quasi-periodic jets, the period of the filament longitudinal oscillations depends also on the driving period of the jets, not simply the pendulum period. With a parameter survey in simulations, we derived a formula, by which one can derive the pendulum oscillation period using the observed period of decayless filament oscillations and the driving periods of jets.

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“…4.2). Magnetic flux emergence is still regarded as an important trigger mechanism for solar jets (Paraschiv et al 2020).…”

Section: 7mentioning

confidence: 99%

Impulsive SEP Events (and Flares)

Reames

2021

Solar Energetic Particles

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Abstract3He-rich, Fe-rich, and enriched in elements with Z > 50, the abundances of solar energetic particles (SEPs) from the small impulsive SEP events stand out as luminaries in our study. The 3He is enhanced by resonant wave-particle interactions. Element abundances increase 1000-fold as the ~3.6 power of the mass-to-charge ratio A/Q from He to heavy elements like Au or Pb, enhanced during acceleration in islands of magnetic reconnection in solar jets, and probably also in flares. This power-law of enhancement vs. A/Q implies Q determined by a source temperature of 2.5–3.2 MK, typical of jets from solar active regions where these impulsive SEPs occur. However, a few small events are unusual; several have suppressed 4He, and rarely, a few very small events with steep spectra have elements N or S greatly enhanced, perhaps by the same resonant-wave mechanism that enhances 3He. Which mechanism will dominate? The impulsive SEP events we see are associated with narrow CMEs, from solar jets where magnetic reconnection on open field lines gives energetic particles and CMEs direct access to space. Gamma-ray lines tell us that the same acceleration physics may occur in flares.

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The Trigger Mechanism of Recurrent Solar Active Region Jets Revealed by the Magnetic Properties of a Coronal Geyser Site

Cited by 12 publications

References 57 publications

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Impulsive SEP Events (and Flares)

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