Dependence of the intensity of the nonwave component of EUV waves on coronal magnetic field configuration
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866918069316616192 |
|---|---|
| author | Li, Yuwei Guo, J. H. Ni, Y. W. Zhang, Z. Y. Chen, P. F. |
| author_facet | Li, Yuwei Guo, J. H. Ni, Y. W. Zhang, Z. Y. Chen, P. F. |
| contents | Context. Mounting evidence has shown that EUV waves consist of a fast-mode magnetohydrodynamic (MHD) wave (or shock wave) followed by a slower nonwave component, as predicted by the magnetic fieldline stretching model. However, not all observed events display both wavefronts, particularly the slower nonwave component. Even in case that the slower nonwave component is present, the intensity distribution often exhibits strong anisotropy.
Aims. This study is intended to unveil the formation condition of the slower nonwave component of EUV waves. Methods. We analyzed the EUV wave event on 8 March 2019, and compared the EUV wave intensity map with the extrapolation coronal potential magnetic field. Data-inspired MHD simulation was also performed.
Results. Two types of EUV waves are identified, and the slower nonwave component exhibits strong anisotropy. By reconstructing 3D coronal magnetic fields, we found that the slower nonwave component of EUV waves is more pronounced in the regions where magnetic fields are backward-inclined, which is further reproduced by our MHD simulations.
Conclusions. The anisotropy of the slower nonwave component of EUV waves is strongly related to the magnetic configuration, with backward-inclined field lines favoring their appearance. The more the field lines are forward-inclined, the weaker such wavelike fronts are. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_11115 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Dependence of the intensity of the nonwave component of EUV waves on coronal magnetic field configuration Li, Yuwei Guo, J. H. Ni, Y. W. Zhang, Z. Y. Chen, P. F. Solar and Stellar Astrophysics Context. Mounting evidence has shown that EUV waves consist of a fast-mode magnetohydrodynamic (MHD) wave (or shock wave) followed by a slower nonwave component, as predicted by the magnetic fieldline stretching model. However, not all observed events display both wavefronts, particularly the slower nonwave component. Even in case that the slower nonwave component is present, the intensity distribution often exhibits strong anisotropy. Aims. This study is intended to unveil the formation condition of the slower nonwave component of EUV waves. Methods. We analyzed the EUV wave event on 8 March 2019, and compared the EUV wave intensity map with the extrapolation coronal potential magnetic field. Data-inspired MHD simulation was also performed. Results. Two types of EUV waves are identified, and the slower nonwave component exhibits strong anisotropy. By reconstructing 3D coronal magnetic fields, we found that the slower nonwave component of EUV waves is more pronounced in the regions where magnetic fields are backward-inclined, which is further reproduced by our MHD simulations. Conclusions. The anisotropy of the slower nonwave component of EUV waves is strongly related to the magnetic configuration, with backward-inclined field lines favoring their appearance. The more the field lines are forward-inclined, the weaker such wavelike fronts are. |
| title | Dependence of the intensity of the nonwave component of EUV waves on coronal magnetic field configuration |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2505.11115 |