Hydrodynamic modeling of tomographically reconstructed coronal loops
The solar corona is structured by the magnetic field in the form of loops or flux tubes. During periods of minimum solar activity or in the quiescent corona (outside active regions), density and temperature inhomogeneities between loops and their surroundings are relatively low, making them not easi...
Guardado en:
| Autores principales: | , , , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2021
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/165203 |
| Aporte de: |
| Sumario: | The solar corona is structured by the magnetic field in the form of loops or flux tubes. During periods of minimum solar activity or in the quiescent corona (outside active regions), density and temperature inhomogeneities between loops and their surroundings are relatively low, making them not easily distinguishable in EUV images. Using differential emission measure tomography, combined with a global potential model of the coronal magnetic field, it is possible to characterize the physical parameters of the plasma along loops built from field lines obtained with the magnetic model. In this work, we use a tomographic reconstruction of the Carrington rotation 2082 to analyze statistically the thermodynamic properties of coronal loops. These results are compared with the ID model, Hydrodynamics and Radiation Code (HYDRAD), for constant or impulsive heating regimes. |
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