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

Nisticò, Giuseppe; Pascoe, D. J.; Nakariakov, V. M.

doi:10.1051/0004-6361/201423763

Cited by 84 publications

(94 citation statements)

References 45 publications

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“…Rather, it is based on the relationship to other periodicities and comparison with those expected for known wave modes when realistic loop and plasma properties are assumed. Zhang et al (2015) reported an observation of a coronal funnel with SDO/AIA which demonstrates fast and slow waves propagating along the same field-aligned path, consistent with numerical simulations of Pascoe et al (2013b; Nisticò et al (2014). Measurement of the propagation speeds allowed the plasma-β to be estimated as approximately 0.01.…”

Section: Introductionsupporting

confidence: 52%

Spatially resolved observation of the fundamental and second harmonic standing kink modes using SDO/AIA

Pascoe

Goddard

Nakariakov

2016

A&A

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Aims. We consider a coronal loop kink oscillation observed by the Atmospheric Imaging Assembly (AIA) of the Solar Dynamics Observatory (SDO) which demonstrates two strong spectral components. The period of the lower frequency component being approximately twice that of the shorter frequency component suggests the presence of harmonics. Methods. We examine the presence of two longitudinal harmonics by investigating the spatial dependence of the loop oscillation. The time-dependent displacement of the loop is measured at 15 locations along the loop axis. For each position the detrended displacement is fitted as the sum of two damped sinusoids, having periods P 1 and P 2 , and a damping time τ. The shorter period component exhibits anti-phase oscillations in the loop legs. Results. We interpret the observation in terms of the first (global or fundamental) and second longitudinal harmonics of the standing kink mode. The strong excitation of the second harmonic appears connected to the preceding coronal mass ejection (CME) which displaced one of the loop legs. The oscillation parameters found are P 1 " 5.00˘0.62 minutes, P 2 " 2.20˘0.23 minutes, P 1 {2P 2 " 1.15˘0.22, and τ{P " 3.35˘1.45.

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Section: Introductionsupporting

confidence: 52%

Spatially resolved observation of the fundamental and second harmonic standing kink modes using SDO/AIA

Pascoe

Goddard

Nakariakov

2016

A&A

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“…A more detailed study of dispersive formation of fast wave trains in plasma funnels strengthened this interpretation (Pascoe et al 2013). Recent studies showed convincing consistence of numerical and observational results (Nisticò et al 2014).…”

Section: Introductionmentioning

confidence: 85%

Coexisting fast and slow propagating waves of the extreme-UV intensity in solar coronal plasma structures

Zhang

Wang

et al. 2015

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Context. From 06:15 UT to 08:15 UT on 2011 June 2, a toroidal filament located at the joint of two active regions, 11226 and 11227, appeared to perform two eruptions. During this phenomenon, fast and slow magnetoacoustic waves were detected to propagate simultaneously along a funnel coronal loop system of AR 11227. Aims. We aim to understand the relationship between fast and slow magnetoacoustic waves during their propagations and measure their properties, such as the propagating speed, path, amplitude, and period observed in the extreme ultraviolet (EUV) wavebands. Methods. We analyse time sequences of EUV images acquired by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. By creating time-distance maps along selected directions, we measure the speeds and localisation of EUV intensity waves in different EUV wavebands. We determine the periods of the waves with wavelet analysis. Results. The fast and slow magnetoacoustic waves, apparently propagating along the same path, are found to have different properties. Their apparent propagation speeds, travel distances, and periods are about 900 km s −1 and 100 km s −1 , 145 Mm and 36 Mm, and 2 min and 3 min, respectively.

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“…3.1. The magnetic field used in our model is a potential field (see also Nisticò et al 2014) given by B " B 0 exp p´y{l 0 q rcos px{l 0 qē x´s in px{l 0 qē y s , (8) where B 0 is a constant determining the magnitude of the field and l 0 is the normalisation factor for the spatial size. The density profile for the field-aligned coronal loop is based on the generalised symmetric Epstein profile (Eq.…”

Section: Numerical Simulations Of Standing Sausage Modes In a Curved mentioning

confidence: 99%

“…For example, Oliver et al (2014) recently studied the dispersive evolution of propagating kink waves in coronal loops. The dispersion of propagating fast MHD waves has also been considered for current sheets (Edwin et al 1986;, coronal holes , and flaring active regions (Nisticò et al 2014) (see also recent review by Pascoe 2014).…”

Section: Introductionmentioning

confidence: 99%

Standing sausage modes in curved coronal slabs

Pascoe

Nakariakov

2016

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

Cited by 84 publications

References 45 publications

Spatially resolved observation of the fundamental and second harmonic standing kink modes using SDO/AIA

Spatially resolved observation of the fundamental and second harmonic standing kink modes using SDO/AIA

Coexisting fast and slow propagating waves of the extreme-UV intensity in solar coronal plasma structures

Standing sausage modes in curved coronal slabs

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