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...

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Detalles Bibliográficos
Publicado: 2005
Materias:
Instabilities
Sun: corona
Sun: magnetic fields
Waves
Magnetic fields
Optical telescopes
Space research
Velocity measurement
Coronal loop structure
Solar system
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v441_n1_p327_Borgazzi
http://hdl.handle.net/20.500.12110/paper_00046361_v441_n1_p327_Borgazzi
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00046361_v441_n1_p327_Borgazzi
record_format dspace
spelling paper:paper_00046361_v441_n1_p327_Borgazzi2023-06-08T14:27:39Z Characterization of intensity and spatial variations along coronal loops: II. A TRACE case study 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. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v441_n1_p327_Borgazzi 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
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.
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
publishDate 2005
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v441_n1_p327_Borgazzi
http://hdl.handle.net/20.500.12110/paper_00046361_v441_n1_p327_Borgazzi
_version_ 1768545489779687424

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