| Full text | |
| Author(s): |
Zurbriggen, Ernesto
[1]
;
Cecere, Mariana
[2, 3]
;
Sieyra, Maria Valeria
[4]
;
Krause, Gustavo
[5, 6]
;
Costa, Andrea
[2]
;
Gimenez de Castro, C. Guillermo
[1]
Total Authors: 6
|
| Affiliation: | [1] Univ Presbiteriana Mackenzie, Ctr Radio Astron & Astrofis Mackenzie CRAAM, Sao Paulo, SP - Brazil
[2] Consejo Nacl Invest Cient & Tecn CONICET, Inst Astron Teor & Expt IATE, Cordoba - Argentina
[3] Univ Nacl Cordoba UNC, Observatorio Astron Cordoba OAC, Cordoba - Argentina
[4] Katholieke Univ Leuven, Dept Math, Ctr Math Plasma Astrophys, Celestijnenlaan 200B, B-3001 Leuven - Belgium
[5] Univ Nacl Cordoba, Fac Ciencias Exactas Fis & Nat, Cordoba - Argentina
[6] Consejo Nacl Invest Cient & Tecn, Inst Estudios Avanzados Ingn & Tecnol IDIT, Cordoba - Argentina
Total Affiliations: 6
|
| Document type: | Journal article |
| Source: | SOLAR PHYSICS; v. 296, n. 12 DEC 2021. |
| Web of Science Citations: | 0 |
| 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. (AU) | |
| FAPESP's process: | 13/24155-3 - Solar flare diagnostic in an unprecedented frequency range from microwaves to THz frequencies: challenges for interpretation (flat) |
| Grantee: | Carlos Guillermo Giménez de Castro |
| Support Opportunities: | Research Projects - Thematic Grants |
| FAPESP's process: | 18/25177-4 - Supra-arcade downflows modelling through its signature at radio and microwaves |
| Grantee: | Ernesto Zurbriggen |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |