Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study
We describe dynamical features and evolutionary characteristics of brightening coronal loops. We describe intensity variations, both in space and time, along a coarse grain loop structure, confirming high speed velocity scenarios. We apply the method to TRACE space-born images that show a compound o...
Guardado en:
Autores principales: | , |
---|---|
Formato: | JOUR |
Materias: | |
Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_00046361_v441_n1_p327_Borgazzi |
Aporte de: |
id |
todo:paper_00046361_v441_n1_p327_Borgazzi |
---|---|
record_format |
dspace |
spelling |
todo:paper_00046361_v441_n1_p327_Borgazzi2023-10-03T14:00:13Z Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study Borgazzi, A. Costa, A. Instabilities Sun: corona Sun: magnetic fields Waves Magnetic fields Optical telescopes Space research Velocity measurement Waves Coronal loop structure Instabilities Sun: corona Sun: magnetic fields Solar system We describe dynamical features and evolutionary characteristics of brightening coronal loops. We describe intensity variations, both in space and time, along a coarse grain loop structure, confirming high speed velocity scenarios. We apply the method to TRACE space-born images that show a compound of several magnetic threads. MICA ground-based images display a unique non-resolved loop structure. We confirm that a coherent behavior of the intensity along neighboring magnetic tubes occurs, i.e. we obtain a similar pattern from both telescopes: each has two branches, suggesting the sliding down of plasma in both directions from a given position on the loop structure. The apparent sliding down occurs in approximately 12 min. After the first appearance, TRACE registers two reiterations of the phenomenon suggesting a wave-based explanation. The feasibility of wave-based and flow-based models is analyzed. In either case, in order to explain the coherent coronal behavior the scenario of apparently non-interacting coronal threads requires theoretical explanations that consider uniform chromospheric conditions covering the footpoints of all the related magnetic tubes. We suggest a characteristic longitude of coherence. © ESO 2005. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v441_n1_p327_Borgazzi |
institution |
Universidad de Buenos Aires |
institution_str |
I-28 |
repository_str |
R-134 |
collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
topic |
Instabilities Sun: corona Sun: magnetic fields Waves Magnetic fields Optical telescopes Space research Velocity measurement Waves Coronal loop structure Instabilities Sun: corona Sun: magnetic fields Solar system |
spellingShingle |
Instabilities Sun: corona Sun: magnetic fields Waves Magnetic fields Optical telescopes Space research Velocity measurement Waves Coronal loop structure Instabilities Sun: corona Sun: magnetic fields Solar system Borgazzi, A. Costa, A. Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study |
topic_facet |
Instabilities Sun: corona Sun: magnetic fields Waves Magnetic fields Optical telescopes Space research Velocity measurement Waves Coronal loop structure Instabilities Sun: corona Sun: magnetic fields Solar system |
description |
We describe dynamical features and evolutionary characteristics of brightening coronal loops. We describe intensity variations, both in space and time, along a coarse grain loop structure, confirming high speed velocity scenarios. We apply the method to TRACE space-born images that show a compound of several magnetic threads. MICA ground-based images display a unique non-resolved loop structure. We confirm that a coherent behavior of the intensity along neighboring magnetic tubes occurs, i.e. we obtain a similar pattern from both telescopes: each has two branches, suggesting the sliding down of plasma in both directions from a given position on the loop structure. The apparent sliding down occurs in approximately 12 min. After the first appearance, TRACE registers two reiterations of the phenomenon suggesting a wave-based explanation. The feasibility of wave-based and flow-based models is analyzed. In either case, in order to explain the coherent coronal behavior the scenario of apparently non-interacting coronal threads requires theoretical explanations that consider uniform chromospheric conditions covering the footpoints of all the related magnetic tubes. We suggest a characteristic longitude of coherence. © ESO 2005. |
format |
JOUR |
author |
Borgazzi, A. Costa, A. |
author_facet |
Borgazzi, A. Costa, A. |
author_sort |
Borgazzi, A. |
title |
Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study |
title_short |
Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study |
title_full |
Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study |
title_fullStr |
Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study |
title_full_unstemmed |
Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study |
title_sort |
characterization of intensity and spatial variations along coronal loops: ii. a trace case study |
url |
http://hdl.handle.net/20.500.12110/paper_00046361_v441_n1_p327_Borgazzi |
work_keys_str_mv |
AT borgazzia characterizationofintensityandspatialvariationsalongcoronalloopsiiatracecasestudy AT costaa characterizationofintensityandspatialvariationsalongcoronalloopsiiatracecasestudy |
_version_ |
1782026008081203200 |