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...

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Autores principales: Mac Cormack, C., López Fuentes, M., Mandrini, Cristina Hemilse, Lloveras, D. G., Vásquez, A. M.
Formato: Articulo
Lenguaje:Inglés
Publicado: 2021
Materias:
Ciencias Astronómicas
Sun: corona
Sun: magnetic fields
Sun: UV radiation
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/165203
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-165203
record_format dspace
spelling I19-R120-10915-1652032024-04-23T20:03:21Z http://sedici.unlp.edu.ar/handle/10915/165203 Hydrodynamic modeling of tomographically reconstructed coronal loops Mac Cormack, C. López Fuentes, M. Mandrini, Cristina Hemilse Lloveras, D. G. Vásquez, A. M. 2021 2024-04-23T16:26:55Z en Ciencias Astronómicas Sun: corona Sun: magnetic fields Sun: UV radiation 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. La estructura de la corona solar se encuentra determinada por la presencia del campo magnético que le da forma a los arcos observados. En épocas de mínimo de actividad solar o en zonas de la corona tranquila (fuera de las regiones activas), las inhomogeneidades en densidad y temperatura entre los arcos y su entorno son relativamente bajas, haciendo que no sean fácilmente distinguibles en imágenes EUV. Utilizando tomografía de medida de emisión diferencial, combinada con modelos potenciales globales del campo magnético coronal, es posible caracterizar parámetros físicos del plasma a lo largo de arcos construidos a partir de líneas de campo obtenidas con el modelo. En este trabajo se utilizó una reconstrucción tomográfica de la rotación de Carrington 2082, para analizar estadísticamente las propiedades termodinámicas de los arcos coronales. Estos resultados se comparan con el modelo ID, Hydrodynamics and Radiation Code (HYDRAD), para regímenes de calentamiento constante o impulsivo. Asociación Argentina de Astronomía Articulo Articulo http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) application/pdf 28-30
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Sun: corona
Sun: magnetic fields
Sun: UV radiation
spellingShingle Ciencias Astronómicas
Sun: corona
Sun: magnetic fields
Sun: UV radiation
Mac Cormack, C.
López Fuentes, M.
Mandrini, Cristina Hemilse
Lloveras, D. G.
Vásquez, A. M.
Hydrodynamic modeling of tomographically reconstructed coronal loops
topic_facet Ciencias Astronómicas
Sun: corona
Sun: magnetic fields
Sun: UV radiation
description 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.
format Articulo
Articulo
author Mac Cormack, C.
López Fuentes, M.
Mandrini, Cristina Hemilse
Lloveras, D. G.
Vásquez, A. M.
author_facet Mac Cormack, C.
López Fuentes, M.
Mandrini, Cristina Hemilse
Lloveras, D. G.
Vásquez, A. M.
author_sort Mac Cormack, C.
title Hydrodynamic modeling of tomographically reconstructed coronal loops
title_short Hydrodynamic modeling of tomographically reconstructed coronal loops
title_full Hydrodynamic modeling of tomographically reconstructed coronal loops
title_fullStr Hydrodynamic modeling of tomographically reconstructed coronal loops
title_full_unstemmed Hydrodynamic modeling of tomographically reconstructed coronal loops
title_sort hydrodynamic modeling of tomographically reconstructed coronal loops
publishDate 2021
url http://sedici.unlp.edu.ar/handle/10915/165203
work_keys_str_mv AT maccormackc hydrodynamicmodelingoftomographicallyreconstructedcoronalloops
AT lopezfuentesm hydrodynamicmodelingoftomographicallyreconstructedcoronalloops
AT mandrinicristinahemilse hydrodynamicmodelingoftomographicallyreconstructedcoronalloops
AT lloverasdg hydrodynamicmodelingoftomographicallyreconstructedcoronalloops
AT vasquezam hydrodynamicmodelingoftomographicallyreconstructedcoronalloops
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