Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24

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The combination of differential emission measure tomography with extrapolation of the photospheric magnetic field allows determination of the electron density and electron temperature along individual magnetic field lines. This is especially useful in quiet-Sun (QS) plasmas where individual loops ca...

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Autores principales: Manchester IV, W.B., Nuevo, F.A., Huang, Z., Frazin, R., Jin, M., Vásquez, A.M.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2013
Materias:
Sun: corona
Sun: evolution
Sun: magnetic topology
Sun: UV radiation
sunspots
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_0004637X_v773_n1_p_ManchesterIV
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paperaa:paper_0004637X_v773_n1_p_ManchesterIV
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spelling paperaa:paper_0004637X_v773_n1_p_ManchesterIV2023-06-12T16:41:08Z Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24 Astrophys. J. 2013;773(1) Manchester IV, W.B. Nuevo, F.A. Huang, Z. Frazin, R. Jin, M. Vásquez, A.M. Sun: corona Sun: evolution Sun: magnetic topology Sun: UV radiation sunspots The combination of differential emission measure tomography with extrapolation of the photospheric magnetic field allows determination of the electron density and electron temperature along individual magnetic field lines. This is especially useful in quiet-Sun (QS) plasmas where individual loops cannot otherwise be identified. In Paper I, this approach was applied to study QS plasmas during Carrington rotation (CR) 2077 at the minimum between solar cycles (SCs) 23 and 24. In that work, two types of QS coronal loops were identified: "up" loops in which the temperature increases with height, and "down" loops in which the temperature decreases with height. While the first ones were expected, the latter ones were a surprise and, furthermore, were found to be ubiquitous in the low-latitude corona. In the present work, we extend the analysis to 11 CRs around the last solar minimum. We found that the "down" population, always located at low latitudes, was maximum at the time when the sunspot number was minimum, and the number of down loops systematically increased during the declining phase of SC-23 and diminished during the rising phase of SC-24. "Down" loops are found to have systematically larger values of β than do "up" loops. These discoveries are interpreted in terms of excitation of Alfvén waves in the photosphere, and mode conversion and damping in the low corona. © 2013. The American Astronomical Society. All rights reserved.. Fil:Nuevo, F.A. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Vásquez, A.M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2013 info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v773_n1_p_ManchesterIV
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
language Inglés
orig_language_str_mv eng
topic Sun: corona
Sun: evolution
Sun: magnetic topology
Sun: UV radiation
sunspots
spellingShingle Sun: corona
Sun: evolution
Sun: magnetic topology
Sun: UV radiation
sunspots
Manchester IV, W.B.
Nuevo, F.A.
Huang, Z.
Frazin, R.
Jin, M.
Vásquez, A.M.
Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
topic_facet Sun: corona
Sun: evolution
Sun: magnetic topology
Sun: UV radiation
sunspots
description The combination of differential emission measure tomography with extrapolation of the photospheric magnetic field allows determination of the electron density and electron temperature along individual magnetic field lines. This is especially useful in quiet-Sun (QS) plasmas where individual loops cannot otherwise be identified. In Paper I, this approach was applied to study QS plasmas during Carrington rotation (CR) 2077 at the minimum between solar cycles (SCs) 23 and 24. In that work, two types of QS coronal loops were identified: "up" loops in which the temperature increases with height, and "down" loops in which the temperature decreases with height. While the first ones were expected, the latter ones were a surprise and, furthermore, were found to be ubiquitous in the low-latitude corona. In the present work, we extend the analysis to 11 CRs around the last solar minimum. We found that the "down" population, always located at low latitudes, was maximum at the time when the sunspot number was minimum, and the number of down loops systematically increased during the declining phase of SC-23 and diminished during the rising phase of SC-24. "Down" loops are found to have systematically larger values of β than do "up" loops. These discoveries are interpreted in terms of excitation of Alfvén waves in the photosphere, and mode conversion and damping in the low corona. © 2013. The American Astronomical Society. All rights reserved..
format Artículo
Artículo
publishedVersion
author Manchester IV, W.B.
Nuevo, F.A.
Huang, Z.
Frazin, R.
Jin, M.
Vásquez, A.M.
author_facet Manchester IV, W.B.
Nuevo, F.A.
Huang, Z.
Frazin, R.
Jin, M.
Vásquez, A.M.
author_sort Manchester IV, W.B.
title Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
title_short Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
title_full Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
title_fullStr Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
title_full_unstemmed Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
title_sort evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24
publishDate 2013
url http://hdl.handle.net/20.500.12110/paper_0004637X_v773_n1_p_ManchesterIV
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AT huangz evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24
AT frazinr evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24
AT jinm evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24
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