Distinct propagating fast wave trains associated with flaring energy releases

Yuan, Ding; Shen, Yuandeng; Liu, Yu; Nakariakov, V. M.; Tan, Baolin; Huang, Jing

doi:10.1051/0004-6361/201321435

Cited by 74 publications

(109 citation statements)

References 38 publications

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“…Previous works on QFP wave trains Shen et al 2013;Shen & Liu 2012;Yuan et al 2013) showed an intimate connection between the formation and propagation of QFP wave trains and the time variability of the flaring energy release. In particular, of interest are quasi-periodic pulsations (QPP) in the flare light curve.…”

Section: Discussionmentioning

confidence: 95%

“…These waves also form wave trains (e.g. Sych et al 2012), but propagate along the apparent magnetic field lines at essentially sub-sonic speeds, and their periods are typically longer than 120 s. Pascoe et al (2013) developed an advanced numerical model for the dispersive evolution of fast MHD waves in an expanding magnetic field generated by an impulsive, spatially localised energy release with a field-aligned density structure which produced results consistent with the observations of Yuan et al (2013).…”

Section: Introductionmentioning

confidence: 80%

“…Other detailed observations are reported by Shen & Liu (2012) and Shen et al (2013), who demonstrated an intimate association with the flare The movies are available in electronic form at http://www.aanda.org energy releases and the role of magnetic loop structures in guiding these waves. Yuan et al (2013) also observed quasiperiodic propagating fast wave trains associated with flaring radio emission. Rapidly propagating waves of the EUV emission intensity disturbances should not be confused with the wellunderstood and analogous slow waves (see, e.g.…”

Section: Introductionmentioning

confidence: 83%

See 2 more Smart Citations

Observation of a high-quality quasi-periodic rapidly propagating wave train using SDO/AIA

Nisticò

Pascoe

Nakariakov

2014

A&A

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Context. We present a new event of quasi-periodic wave trains observed in EUV wavebands that rapidly propagate away from an active region after a flare. Aims. We measured the parameters of a wave train observed on 7 December 2013 after an M1.2 flare, such as the phase speeds, periods and wavelengths, in relationship to the local coronal environment and the energy sources. Methods. We compared our observations with a numerical simulation of fast magnetoacoustic waves that undergo dispersive evolution and leakage in a coronal loop embedded in a potential magnetic field. Results. The wave train is observed to propagate as several arc-shaped intensity disturbances for almost half an hour, with a speed greater than 1000 km s −1 and a period of about 1 min. The wave train followed two different patterns of propagation, in accordance with the magnetic structure of the active region. The oscillatory signal is found to be of high-quality, i.e. there is a large number (10 or more) of subsequent wave fronts observed. The observations are found to be consistent with the numerical simulation of a fast wave train generated by a localised impulsive energy release. Conclusions. Transverse structuring in the corona can efficiently create and guide high-quality quasi-periodic propagating fast wave trains.

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Section: Discussionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 80%

Section: Introductionmentioning

confidence: 83%

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Observation of a high-quality quasi-periodic rapidly propagating wave train using SDO/AIA

Nisticò

Pascoe

Nakariakov

2014

A&A

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“…MAG waves with frequencies below the cut-off value become evanescent and cannot reach the upper layers of the solar atmosphere. The cut-off value also determines the oscillation frequency of MAG waves excited by a broad-band (i.e., impulsive) source and their propagation to the corona (e.g., Suematsu et al 1982;Botha et al 2011;Yuan et al 2013). The cut-off frequency of MAG waves in a stratified isothermal atmosphere permeated by a uniform magnetic field was derived analytically in Bel & Leroy (1977) and Zhugzhda & Dzhalilov (1984).…”

Section: Introductionmentioning

confidence: 99%

Multi-height observations of magnetoacoustic cut-off frequency in a sunspot atmosphere

Yuan

Сыч

Reznikova

et al. 2013

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Context. The cut-off frequency of magnetoacoustic gravity (MAG) waves could be decreased by the inclined magnetic field, and therefore, low-frequency waves could penetrate into the upper atmosphere. Aims. We observe the distribution of the cut-off frequency of compressive waves at various heights and reconstruct the magnetic field inclination, according to the MAG wave theory in a stratified atmosphere permeated by a uniform magnetic field. Methods. We analysed the emission intensity oscillations of sunspot AR11131 (08 Dec. 2010) observed at the 1700 Å, 1600 Å, and 304 Å bandpasses of the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO), and computed the narrow-band power maps with the pixelised wavelet filtering method. The distribution of the cut-off frequency was defined as the median contour in the azimuthally-averaged oscillation power. The magnetic field inclination was estimated with the local cut-off frequency according to the MAG wave theory in the low-β limit and was compared to the potential field extrapolation. Results. Shorter period oscillations dominate in the sunspot umbra, while longer period oscillations form an annular shape approximately concentric with the sunspot. Oscillations with longer periods are distributed further away from the sunspot centre. The 5 min oscillations appear to originate at or lower than the photosphere. The magnetic field inclinations determined with the cut-off frequency theory are about 30−40% larger than the values obtained by the potential field extrapolation. Conclusions. The oscillation power distribution in a sunspot atmosphere reflects its magnetic and thermal structure. The cut-off frequency could be used to probe the magnetic field inclination, however, other factors have to be included to fully understand this phenomenon. The existence of return magnetic flux at the outer penumbra was evidenced by the cut-off frequency distribution.

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“…This process was described by Roberts et al (1983Roberts et al ( , 1984; Murawski & Roberts (1994); Nakariakov & Roberts (1995) and later observed with instruments such as the Solar Eclipse Coronal Imaging System (SECIS) (Katsiyannis et al 2003;Cooper et al 2003) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO; e.g. Shen & Liu 2012;Liu et al 2012;Yuan et al 2013). The dispersion arises due to the presence of a characteristic transverse length scale and occurs for both sausage (m " 0) and kink (m " 1) fast modes.…”

Section: Introductionmentioning

confidence: 99%

Standing sausage modes in curved coronal slabs

Pascoe

Nakariakov

2016

A&A

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Context. Magnetohydrodynamic waveguides such as dense coronal loops can support standing modes. The ratios of the periods of oscillations for different longitudinal harmonics depend on the dispersive nature of the waveguide and so may be used as a seismological tool to determine coronal parameters. Aims. We extend models of standing sausage modes in low β coronal loops to include the effects of loop curvature. The behaviour of standing sausage modes in this geometry is used to explain the properties of observed oscillations which cannot be accounted for using straight loop models. Methods. We perform 2D numerical simulations of an oscillating coronal loop, modelled as a dense slab embedded in a potential magnetic field. The loop is field-aligned and so experiences expansion with height in addition to being curved. Standing sausage modes are excited by compressive perturbations of the loop and their properties are studied. Results. The spatial profiles of standing sausage modes are found to be modified by the expanding loop geometry typical for flaring loops and modelled by a potential magnetic field in our simulations. Longitudinal harmonics of order n ą 1 have antinodes which are shifted towards the loop apex and the amplitude of antinodes near the loop apex is smaller than those near the loop footpoints. Conclusions. We find that the observation of standing sausage modes by Nakariakov et al. (2003) is consistent with interpretation in terms of the global mode (n " 1) and third harmonic (n " 3). This interpretation accounts for the period ratio and spatial structure of the observed oscillations.

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Distinct propagating fast wave trains associated with flaring energy releases

Cited by 74 publications

References 38 publications

Observation of a high-quality quasi-periodic rapidly propagating wave train using SDO/AIA

Observation of a high-quality quasi-periodic rapidly propagating wave train using SDO/AIA

Multi-height observations of magnetoacoustic cut-off frequency in a sunspot atmosphere

Standing sausage modes in curved coronal slabs

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