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:	JOUR
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	todo:paper_0004637X_v773_n1_p_ManchesterIV
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spelling	todo:paper_0004637X_v773_n1_p_ManchesterIV2023-10-03T14:02:33Z Evolution of the global temperature structure of the solar corona during the minimum between solar cycles 23 and 24 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. JOUR 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)
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	JOUR
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
url	http://hdl.handle.net/20.500.12110/paper_0004637X_v773_n1_p_ManchesterIV
work_keys_str_mv	AT manchesterivwb evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24 AT nuevofa evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24 AT huangz evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24 AT frazinr evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24 AT jinm evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24 AT vasquezam evolutionoftheglobaltemperaturestructureofthesolarcoronaduringtheminimumbetweensolarcycles23and24
_version_	1807314879233654784

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

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