Numerical simulations of the attenuation of the fundamental slow magnetoacoustic standing mode in a gravitationally stratified solar coronal arcade

Konkol, P.; Murawski, K.; Lee, D.; Weide, Klaus

doi:10.1051/0004-6361/201014367

Cited by 11 publications

(11 citation statements)

References 29 publications

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“…The majority of two-dimensional studies of coronal slow waves (e.g. Selwa et al 2007;Ogrodowczyk et al 2009;Konkol et al 2010) addressed the effects of stratification and magnetic field curvature, and hence were carried out in the plane perpendicular to the solar surface. On the other hand, the study of the slow wave progression in the direction perpendicular to the magnetic field in, e.g., two-ribbon flare arcades, requires their modelling in the plane parallel to the solar surface.…”

Section: Introductionmentioning

confidence: 99%

Slow magnetacoustic waves in magnetic arcades

Gruszecki

Nakariakov

2011

A&A

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Aims. We investigate two-dimensional effects on the evolution of impulsively-generated slow magnetoacoustic waves in magnetic arcades of the solar corona. Methods. We used a two-dimensional box model of a coronal arcade, neglecting the effects of gravity and magnetic curvature. Ideal finite-β magnetohydrodynamic equations were employed. The plasma was taken to be uniform, penetrated by a straight and uniform magnetic field. We applied line-tying boundary conditions at the magnetic footpoints. Results. Running and standing slow magnetoacoustic waves develop across the magnetic field due to the reflection from the footpoints in the arcade. The perpendicular group speed is lower than both sound and Alfvén speeds. The speed grows with the increase in plasma-β, which is consistent with analytical theory. Slow magnetoacoustic pulse perturbs the magnetic field and current density; this effect is stronger for higher amplitudes. Standing waves spread across the field, forming a characteristic phase-mixing pattern of antiparallel flows. The two-dimensional effects are more pronounced for higher β. Our results confirm the plausibility of the interpretation of the observed evolution of two-ribbon flares in terms of slow magnetoacoustic waves in magnetic arcades.

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Section: Introductionmentioning

confidence: 99%

Slow magnetacoustic waves in magnetic arcades

Gruszecki

Nakariakov

2011

A&A

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“…The current-free magnetic field (8) has always corresponding scalar field φ e (x, y), and we can deduce the magnetic flux function given as follows (Konkol et al 2010):…”

Section: Initial Conditionsmentioning

confidence: 99%

Velocity Response of the Observed Explosive Events in the Lower Solar Atmosphere: I. Formation of the Flowing Cool Loop System

Srivastava,

Rao,

Konkol

et al. 2020

Preprint

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We observe plasma flows in cool loops using the Slit-Jaw Imager (SJI) onboard the Interface Region Imaging Spectrometer (IRIS). Huang et al. (2015) observed unusually broadened Si IV 1403 Å line profiles at the footpoints of such loops that were attributed to signatures of explosive events (EEs). We have chosen one such uni-directional flowing cool loop system observed by IRIS where one of the footpoints is associated with significantly broadened Si IV line profiles. The line profile broadening indirectly indicates the occurrence of numerous EEs below the transition region (TR), while it directly infers a large velocity enhancement/perturbation further causing the plasma flows in the observed loop system. The observed features are implemented in a model atmosphere in which a low-lying bi-polar magnetic field system is perturbed in the chromosphere by a velocity pulse with a maximum amplitude of 200 km s −1 . The data-driven 2-D numerical simulation shows that the plasma motions evolve in a similar manner as observed by IRIS in the form of flowing plasma filling the skeleton of a cool loop system. We compare the spatio-temporal evolution of the cool loop system in the framework of our model with the observations, and conclude that their formation is mostly associated with the velocity response of the transient energy release above their footpoints in the chromosphere/TR. Our observations and modeling results suggest that the velocity responses most likely associated to the EEs could be one of the main candidates for the dynamics and energetics of the flowing cool loop systems in the lower solar atmosphere.

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“…Konkol et al (2010) evolved a 2D potential arcade in a gravitationally stratified corona, in order to explore the influence of thermal conduction on the attenuation of the fundamental stationary slow magnetoacoustic modes. Moreover, Murawski et al (2011) simulated the formation of macrospicules created by a localized pulse below the transition region.…”

Section: Introductionmentioning

confidence: 99%

Magnus: A New Resistive MHD Code with Heat Flow Terms

Navarro

Lora-Clavijo

González

2017

ApJ

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We present a new magnetohydrodynamic (MHD) code for the simulation of wave propagation in the solar atmosphere, under the effects of electrical resistivity -but not dominant-and heat transference in a uniform 3D grid. The code is based on the finite volume method combined with the HLLE and HLLC approximate Riemann solvers, which use different slope limiters like MINMOD, MC, and WENO5. In order to control the growth of the divergence of the magnetic field, due to numerical errors, we apply the Flux Constrained Transport method, which is described in detail to understand how the resistive terms are included in the algorithm. In our results, it is verified that this method preserves the divergence of the magnetic fields within the machine round-off error (∼ 1 × 10 −12 ). For the validation of the accuracy and efficiency of the schemes implemented in the code, we present some numerical tests in 1D and 2D for the ideal MHD. Later, we show one test for the resistivity in a magnetic reconnection process and one for the thermal conduction, where the temperature is advected by the magnetic field lines. Moreover, we display two numerical problems associated with the MHD wave propagation. The first one corresponds to a 3D evolution of a vertical velocity pulse at the photosphere-transition-corona region, while the second one consists in a 2D simulation of a transverse velocity pulse in a coronal loop.

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Numerical simulations of the attenuation of the fundamental slow magnetoacoustic standing mode in a gravitationally stratified solar coronal arcade

Cited by 11 publications

References 29 publications

Slow magnetacoustic waves in magnetic arcades

Slow magnetacoustic waves in magnetic arcades

Velocity Response of the Observed Explosive Events in the Lower Solar Atmosphere: I. Formation of the Flowing Cool Loop System

Magnus: A New Resistive MHD Code with Heat Flow Terms

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