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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/651
Ver los metadatos del registro completo
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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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1844614319321382912 |
score |
13.070432 |