The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field
- Autores
- van Driel Gesztelyi, Lidia; Démoulin, Pascal; Mandrini, Cristina Hemilse; Harra, L. K.; Klimchuk, J. A.
- Año de publicación
- 2003
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We analyze the evolution of the fluxes observed in X-rays and correlate them with the magnetic flux density in active region (AR) NOAA 7978 from its birth throughout its decay, for five solar rotations. We use Solar and Heliospheric Observatory Michelson Doppler Imager (MDI) data, together with Yohkoh Soft X-Ray Telescope (SXT) and Yohkoh Bragg Crystal Spectrometer (BCS) data, to determine the global evolution of the temperature and the emission measure of the coronal plasma at times when no significant brightenings were observed. We show that the mean X-ray flux and derived parameters, temperature and emission measure (together with other quantities deduced from them, such as the density and the pressure), of the plasma in the AR follow power-law relationships with the mean magnetic flux density (B ). The exponents (b) of these power-law functions (aB b) are derived using two different statistical methods, a classical least-squares method in log-log plots and a nonparametric method, which takes into account the fact that errors in the data may not be normally distributed. Both methods give similar exponents, within error bars, for the mean temperature and for both instruments (SXT and BCS); in particular, b stays in the range [0.27, 0.31] and [0.24, 0.57] for full-resolution SXT images and BCS data, respectively. For the emission measure, the exponent b lies in the range [0.85, 1.35] and [0.45, 1.96] for SXT and BCS, respectively. The determination of such power-law relations, when combined with the results from coronal heating models, can provide us with powerful tools for determining the mechanism responsible for the existence of the high-temperature corona
Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido
Fil: Klimchuk, J. A.. Spece Sciences División. Naval Research Laboratory; Estados Unidos - Materia
- Solar Corona
- 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:11336/21174
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The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic fieldvan Driel Gesztelyi, LidiaDémoulin, PascalMandrini, Cristina HemilseHarra, L. K.Klimchuk, J. A.Solar Coronahttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We analyze the evolution of the fluxes observed in X-rays and correlate them with the magnetic flux density in active region (AR) NOAA 7978 from its birth throughout its decay, for five solar rotations. We use Solar and Heliospheric Observatory Michelson Doppler Imager (MDI) data, together with Yohkoh Soft X-Ray Telescope (SXT) and Yohkoh Bragg Crystal Spectrometer (BCS) data, to determine the global evolution of the temperature and the emission measure of the coronal plasma at times when no significant brightenings were observed. We show that the mean X-ray flux and derived parameters, temperature and emission measure (together with other quantities deduced from them, such as the density and the pressure), of the plasma in the AR follow power-law relationships with the mean magnetic flux density (B ). The exponents (b) of these power-law functions (aB b) are derived using two different statistical methods, a classical least-squares method in log-log plots and a nonparametric method, which takes into account the fact that errors in the data may not be normally distributed. Both methods give similar exponents, within error bars, for the mean temperature and for both instruments (SXT and BCS); in particular, b stays in the range [0.27, 0.31] and [0.24, 0.57] for full-resolution SXT images and BCS data, respectively. For the emission measure, the exponent b lies in the range [0.85, 1.35] and [0.45, 1.96] for SXT and BCS, respectively. The determination of such power-law relations, when combined with the results from coronal heating models, can provide us with powerful tools for determining the mechanism responsible for the existence of the high-temperature coronaFil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Harra, L. K.. Mullard Space Science Laboratory; Reino UnidoFil: Klimchuk, J. A.. Spece Sciences División. Naval Research Laboratory; Estados UnidosIOP Publishing2003-03-20info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21174van Driel Gesztelyi, Lidia; Démoulin, Pascal; Mandrini, Cristina Hemilse; Harra, L. K.; Klimchuk, J. A.; The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field; IOP Publishing; Astrophysical Journal; 586; 1; 20-3-2003; 579-5910004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/367633info:eu-repo/semantics/altIdentifier/doi/10.1086/367633info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:23:43Zoai:ri.conicet.gov.ar:11336/21174instacron: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 10:23:44.265CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
title |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
spellingShingle |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field van Driel Gesztelyi, Lidia Solar Corona |
title_short |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
title_full |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
title_fullStr |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
title_full_unstemmed |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
title_sort |
The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field |
dc.creator.none.fl_str_mv |
van Driel Gesztelyi, Lidia Démoulin, Pascal Mandrini, Cristina Hemilse Harra, L. K. Klimchuk, J. A. |
author |
van Driel Gesztelyi, Lidia |
author_facet |
van Driel Gesztelyi, Lidia Démoulin, Pascal Mandrini, Cristina Hemilse Harra, L. K. Klimchuk, J. A. |
author_role |
author |
author2 |
Démoulin, Pascal Mandrini, Cristina Hemilse Harra, L. K. Klimchuk, J. A. |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
Solar Corona |
topic |
Solar Corona |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
We analyze the evolution of the fluxes observed in X-rays and correlate them with the magnetic flux density in active region (AR) NOAA 7978 from its birth throughout its decay, for five solar rotations. We use Solar and Heliospheric Observatory Michelson Doppler Imager (MDI) data, together with Yohkoh Soft X-Ray Telescope (SXT) and Yohkoh Bragg Crystal Spectrometer (BCS) data, to determine the global evolution of the temperature and the emission measure of the coronal plasma at times when no significant brightenings were observed. We show that the mean X-ray flux and derived parameters, temperature and emission measure (together with other quantities deduced from them, such as the density and the pressure), of the plasma in the AR follow power-law relationships with the mean magnetic flux density (B ). The exponents (b) of these power-law functions (aB b) are derived using two different statistical methods, a classical least-squares method in log-log plots and a nonparametric method, which takes into account the fact that errors in the data may not be normally distributed. Both methods give similar exponents, within error bars, for the mean temperature and for both instruments (SXT and BCS); in particular, b stays in the range [0.27, 0.31] and [0.24, 0.57] for full-resolution SXT images and BCS data, respectively. For the emission measure, the exponent b lies in the range [0.85, 1.35] and [0.45, 1.96] for SXT and BCS, respectively. The determination of such power-law relations, when combined with the results from coronal heating models, can provide us with powerful tools for determining the mechanism responsible for the existence of the high-temperature corona Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido Fil: Klimchuk, J. A.. Spece Sciences División. Naval Research Laboratory; Estados Unidos |
description |
We analyze the evolution of the fluxes observed in X-rays and correlate them with the magnetic flux density in active region (AR) NOAA 7978 from its birth throughout its decay, for five solar rotations. We use Solar and Heliospheric Observatory Michelson Doppler Imager (MDI) data, together with Yohkoh Soft X-Ray Telescope (SXT) and Yohkoh Bragg Crystal Spectrometer (BCS) data, to determine the global evolution of the temperature and the emission measure of the coronal plasma at times when no significant brightenings were observed. We show that the mean X-ray flux and derived parameters, temperature and emission measure (together with other quantities deduced from them, such as the density and the pressure), of the plasma in the AR follow power-law relationships with the mean magnetic flux density (B ). The exponents (b) of these power-law functions (aB b) are derived using two different statistical methods, a classical least-squares method in log-log plots and a nonparametric method, which takes into account the fact that errors in the data may not be normally distributed. Both methods give similar exponents, within error bars, for the mean temperature and for both instruments (SXT and BCS); in particular, b stays in the range [0.27, 0.31] and [0.24, 0.57] for full-resolution SXT images and BCS data, respectively. For the emission measure, the exponent b lies in the range [0.85, 1.35] and [0.45, 1.96] for SXT and BCS, respectively. The determination of such power-law relations, when combined with the results from coronal heating models, can provide us with powerful tools for determining the mechanism responsible for the existence of the high-temperature corona |
publishDate |
2003 |
dc.date.none.fl_str_mv |
2003-03-20 |
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/11336/21174 van Driel Gesztelyi, Lidia; Démoulin, Pascal; Mandrini, Cristina Hemilse; Harra, L. K.; Klimchuk, J. A.; The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field; IOP Publishing; Astrophysical Journal; 586; 1; 20-3-2003; 579-591 0004-637X CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/21174 |
identifier_str_mv |
van Driel Gesztelyi, Lidia; Démoulin, Pascal; Mandrini, Cristina Hemilse; Harra, L. K.; Klimchuk, J. A.; The long-term evolution of AR 7978: The scalings of the coronal plasma parameters with the mean photospheric magnetic field; IOP Publishing; Astrophysical Journal; 586; 1; 20-3-2003; 579-591 0004-637X CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/367633 info:eu-repo/semantics/altIdentifier/doi/10.1086/367633 |
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 |
publisher.none.fl_str_mv |
IOP Publishing |
dc.source.none.fl_str_mv |
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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1844614232970100736 |
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13.070432 |