Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24

Autores
Nuevo, Federico Alberto; Huang, Zhenguang; Frazin, Richard A.; Manchester IV, Ward B.; Jin, Meng; Vasquez, Alberto Marcos
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photospheric magnetic field allows determinatio/n 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 (Huang et al. 2012), this approach was applied to study QS plasmas during Carrington rotation (CR) 2077, at the minimum between solar cycles (SC)-23 and 24. In that work, two types of quiet 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 find 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 $eta$ than do ``up´´ loops. These discoveries are interpreted in terms of excitation of Alfv´en waves in the photosphere, and mode conversion and damping in the low corona.
Fil: Nuevo, Federico Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Huang, Zhenguang. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Frazin, Richard A.. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Manchester IV, Ward B.. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Jin, Meng. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Vasquez, Alberto Marcos. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fuente
© 2013. The American Astronomical Society.
Materia
Sun: Corona
Sun: Magnetic Topology
Sun: Uv Radiation
Sun: Evolution - Sunspots
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/651

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spelling Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24Nuevo, Federico AlbertoHuang, ZhenguangFrazin, Richard A.Manchester IV, Ward B.Jin, MengVasquez, Alberto MarcosSun: CoronaSun: Magnetic TopologySun: Uv RadiationSun: Evolution - Sunspotshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photospheric magnetic field allows determinatio/n 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 (Huang et al. 2012), this approach was applied to study QS plasmas during Carrington rotation (CR) 2077, at the minimum between solar cycles (SC)-23 and 24. In that work, two types of quiet 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 find 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 $eta$ than do ``up´´ loops. These discoveries are interpreted in terms of excitation of Alfv´en waves in the photosphere, and mode conversion and damping in the low corona.Fil: Nuevo, Federico Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); ArgentinaFil: Huang, Zhenguang. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;Fil: Frazin, Richard A.. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;Fil: Manchester IV, Ward B.. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;Fil: Jin, Meng. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;Fil: Vasquez, Alberto Marcos. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); ArgentinaIop Publishing Ltd2013-07-19info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/651Nuevo, Federico Alberto; Huang, Zhenguang; Frazin, Richard A.; Manchester IV, Ward B.; Jin, Meng; et al.; Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24; Iop Publishing Ltd; Astrophysical Journal; 773; 9; 19-7-2013; 14pp0004-637X© 2013. The American Astronomical Society.reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicasenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/773/1/9info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/773/1/9/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/2025-09-29T10:31:00Zoai:ri.conicet.gov.ar:11336/651instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:31:00.981CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24
title Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24
spellingShingle Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24
Nuevo, Federico Alberto
Sun: Corona
Sun: Magnetic Topology
Sun: Uv Radiation
Sun: Evolution - Sunspots
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
dc.creator.none.fl_str_mv Nuevo, Federico Alberto
Huang, Zhenguang
Frazin, Richard A.
Manchester IV, Ward B.
Jin, Meng
Vasquez, Alberto Marcos
author Nuevo, Federico Alberto
author_facet Nuevo, Federico Alberto
Huang, Zhenguang
Frazin, Richard A.
Manchester IV, Ward B.
Jin, Meng
Vasquez, Alberto Marcos
author_role author
author2 Huang, Zhenguang
Frazin, Richard A.
Manchester IV, Ward B.
Jin, Meng
Vasquez, Alberto Marcos
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Sun: Corona
Sun: Magnetic Topology
Sun: Uv Radiation
Sun: Evolution - Sunspots
topic Sun: Corona
Sun: Magnetic Topology
Sun: Uv Radiation
Sun: Evolution - Sunspots
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photospheric magnetic field allows determinatio/n 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 (Huang et al. 2012), this approach was applied to study QS plasmas during Carrington rotation (CR) 2077, at the minimum between solar cycles (SC)-23 and 24. In that work, two types of quiet 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 find 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 $eta$ than do ``up´´ loops. These discoveries are interpreted in terms of excitation of Alfv´en waves in the photosphere, and mode conversion and damping in the low corona.
Fil: Nuevo, Federico Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Huang, Zhenguang. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Frazin, Richard A.. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Manchester IV, Ward B.. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Jin, Meng. Department of Atmospheric, Oceanic and Space Sciences. University of Michigan; Estados Unidos de América;
Fil: Vasquez, Alberto Marcos. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
description The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photospheric magnetic field allows determinatio/n 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 (Huang et al. 2012), this approach was applied to study QS plasmas during Carrington rotation (CR) 2077, at the minimum between solar cycles (SC)-23 and 24. In that work, two types of quiet 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 find 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 $eta$ than do ``up´´ loops. These discoveries are interpreted in terms of excitation of Alfv´en waves in the photosphere, and mode conversion and damping in the low corona.
publishDate 2013
dc.date.none.fl_str_mv 2013-07-19
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/651
Nuevo, Federico Alberto; Huang, Zhenguang; Frazin, Richard A.; Manchester IV, Ward B.; Jin, Meng; et al.; Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24; Iop Publishing Ltd; Astrophysical Journal; 773; 9; 19-7-2013; 14pp
0004-637X
url http://hdl.handle.net/11336/651
identifier_str_mv Nuevo, Federico Alberto; Huang, Zhenguang; Frazin, Richard A.; Manchester IV, Ward B.; Jin, Meng; et al.; Evolution of the Global Temperature Structure of the Solar Corona During the Minimum between Solar Cycles 23 and 24; Iop Publishing Ltd; Astrophysical Journal; 773; 9; 19-7-2013; 14pp
0004-637X
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/773/1/9
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/773/1/9/meta
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Iop Publishing Ltd
publisher.none.fl_str_mv Iop Publishing Ltd
dc.source.none.fl_str_mv © 2013. The American Astronomical Society.
reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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