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An MHD Study of Large-Amplitude Oscillations in Solar Filaments

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Abstract

Quiescent filaments are usually affected by internal and/or external perturbations triggering oscillations of different kinds. In particular, external large-scale coronal waves can perturb remote quiescent filaments leading to large-amplitude oscillations. Observational reports have indicated that the activation time of oscillations coincides with the passage of a large-scale coronal wavefront through the filament, although the disturbing wave is not always easily detected. Aiming to contribute to understanding how –and to what extent– coronal waves are able to excite filament oscillations, here we modelled with 2.5D magnetohydrodynamic simulations a filament floating in a gravitationally stratified corona disturbed by a coronal shock wave. This simplified scenario results in a two-coupled-oscillation pattern of the filament, which is damped in a few cycles, enabling a detailed analysis. A parametric study was carried out varying parameters of the scenario such as height, size, and mass of the filament. An oscillatory analysis reveals a general tendency for periods of oscillations, amplitudes, and damping times to increase with height, whereas filaments of larger radius exhibit shorter periods and smaller amplitudes. The calculation of forces exerted on the filament shows that the main restoring force is the magnetic tension.

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Acknowledgements

We want to thank an anonymous reviewer who helped us to make a significant improvement to this work. E. Zurbriggen is grateful to the FAPESP to have financed this research by the grant 2018/25177-4. M. Cécere, G. Krause, and A. Costa are members of the Carrera del Investigador Científico (CONICET). M. Cécere and G. Krause acknowledge support from ANPCyT under the grant PICT No. 2016-2480. M. Cécere also acknowledges support from the SECYT-UNC grant No. 33620180101147CB. M.V. Sieyra acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 724326). C.G.G. Castro thanks CNPq for support with a Productivity Research Fellowship. The research leading to these results has received funding from CAPES grant 88881.310386/2018-01, FAPESP grant 2013/24155-3. E. Zurbriggen and C.G.G. Castro are also grateful to Mackenzie Research Funding Mackpesquisa for the support received. C.G.G. Castro is Correspondent Researcher of the CONICET for the Instituto de Astronomía y Física del Espacio (IAFE), Argentina. Simulations were run on the IATE’s clusters and CRAAM’s cluster wintermute; we thank system managers D. Graña and T. Giorgetti. The software used in this work was developed in part by the DOE NNSA ASC- and DOE Office of Science ASCR-supported Flash Center for Computational Science at the University of Chicago (Flash code). We also thank the VisIt team for developing the graphical tool used in this work (Harrison and Krishnan, 2012).

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Authors and Affiliations

  1. Centro de Rádio Astronomia e Astrofísica Mackenzie (CRAAM), Universidade Presbiteriana Mackenzie, SP, São Paulo, Brazil

    Ernesto Zurbriggen & C. Guillermo Giménez de Castro

  2. Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Instituto de Astronomía Teórica y Experimental (IATE), Córdoba, Argentina

    Mariana Cécere & Andrea Costa

  3. Observatorio Astronómico de Córdoba (OAC), Universidad Nacional de Córdoba (UNC), Córdoba, Argentina

    Mariana Cécere

  4. Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001, Leuven, Belgium

    María Valeria Sieyra

  5. Consejo Nacional de Investigaciones Científicas y Técnicas, Instituto de Estudios Avanzados en Ingeniería y Tecnología (IDIT), Córdoba, Argentina

    Gustavo Krause

  6. Facultad de Ciencias Exactas, Físicas y Naturales, Universidad Nacional de Córdoba, Córdoba, Argentina

    Gustavo Krause

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  1. Ernesto Zurbriggen
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  2. Mariana Cécere
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  3. María Valeria Sieyra
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  4. Gustavo Krause
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  6. C. Guillermo Giménez de Castro
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Correspondence to Ernesto Zurbriggen.

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Magnetohydrodynamic (MHD) Waves and Oscillations in the Sun’s Corona and MHD Coronal Seismology

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Zurbriggen, E., Cécere, M., Sieyra, M.V. et al. An MHD Study of Large-Amplitude Oscillations in Solar Filaments. Sol Phys 296, 173 (2021). https://doi.org/10.1007/s11207-021-01908-z

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