Modeling the Mg I from the NUV to MIR. I. The solar case
- Autores
- Peralta, Juan Ignacio; Vieytes, Mariela Cristina; Mendez, Marta Patricia Alejandra; Mitnik, Dario Marcelo
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Semi-empirical models of the solar atmosphere are used to study the radiative environment of any planet in our Solar System. There is a need for reliable atomic data for neutral atoms and ions in the atmosphere to obtain improved calculated spectra. Atomic parameters are crucial to computing the correct population of elements through the whole stellar atmosphere. Although there is very good agreement between the observed and calculated spectra for the Sun, there is still a mismatch in several spectral ranges due to the lack of atomic data and the inaccuracies thereof, particularly for neutrals such as Mga» I. Aims. To represent many spectral lines of Mga» I from the near-ultraviolet to the mid-infrared correctly, it is necessary to add and update the atomic data involved in the atomic processes that drive their formation. Methods. The improvements made to the Mga» I atomic model are as follows: i) 127 strong lines, including their broadening data, were added. ii) To obtain these new lines, we increased the number of energy levels from 26 to 85. iii) Photoionization cross-section parameters were added and updated. iv) Effective collision strength (I' ij ) parameters were updated for the first 25 levels using the existing data from the convergent close-coupling calculations. One of the most significant changes in our model is given by the new I' ij parameters for transitions involving levels between 26 and 54, which were computed with a multiconfiguration Breit-Pauli distorted-wave (DW) method. For transitions involving superlevels, we calculated the I' ij parameters with the usual semi-empirical formulas. Results. More than 100 transitions were added to our calculations, increasing our capability of reproducing important features observed in the solar spectra. We found a remarkable improvement in matching the solar spectra for wavelengths higher than 30 000 Å when our new DW I' ij data were used in the model.
Fil: Peralta, Juan Ignacio. Universidad Nacional de Tres de Febrero; Argentina. Consejo Nacional de Investigaciones 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: Vieytes, Mariela Cristina. Universidad Nacional de Tres de Febrero; Argentina. Consejo Nacional de Investigaciones 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: Mendez, Marta Patricia Alejandra. Consejo Nacional de Investigaciones 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: Mitnik, Dario Marcelo. Consejo Nacional de Investigaciones 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 - Materia
-
ATOMIC DATA
LINE: FORMATION
LINE: PROFILES
SUN: ATMOSPHERE
SUN: INFRARED - 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:11336/182597
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Modeling the Mg I from the NUV to MIR. I. The solar casePeralta, Juan IgnacioVieytes, Mariela CristinaMendez, Marta Patricia AlejandraMitnik, Dario MarceloATOMIC DATALINE: FORMATIONLINE: PROFILESSUN: ATMOSPHERESUN: INFRAREDhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Semi-empirical models of the solar atmosphere are used to study the radiative environment of any planet in our Solar System. There is a need for reliable atomic data for neutral atoms and ions in the atmosphere to obtain improved calculated spectra. Atomic parameters are crucial to computing the correct population of elements through the whole stellar atmosphere. Although there is very good agreement between the observed and calculated spectra for the Sun, there is still a mismatch in several spectral ranges due to the lack of atomic data and the inaccuracies thereof, particularly for neutrals such as Mga» I. Aims. To represent many spectral lines of Mga» I from the near-ultraviolet to the mid-infrared correctly, it is necessary to add and update the atomic data involved in the atomic processes that drive their formation. Methods. The improvements made to the Mga» I atomic model are as follows: i) 127 strong lines, including their broadening data, were added. ii) To obtain these new lines, we increased the number of energy levels from 26 to 85. iii) Photoionization cross-section parameters were added and updated. iv) Effective collision strength (I' ij ) parameters were updated for the first 25 levels using the existing data from the convergent close-coupling calculations. One of the most significant changes in our model is given by the new I' ij parameters for transitions involving levels between 26 and 54, which were computed with a multiconfiguration Breit-Pauli distorted-wave (DW) method. For transitions involving superlevels, we calculated the I' ij parameters with the usual semi-empirical formulas. Results. More than 100 transitions were added to our calculations, increasing our capability of reproducing important features observed in the solar spectra. We found a remarkable improvement in matching the solar spectra for wavelengths higher than 30 000 Å when our new DW I' ij data were used in the model.Fil: Peralta, Juan Ignacio. Universidad Nacional de Tres de Febrero; Argentina. Consejo Nacional de Investigaciones 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: Vieytes, Mariela Cristina. Universidad Nacional de Tres de Febrero; Argentina. Consejo Nacional de Investigaciones 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: Mendez, Marta Patricia Alejandra. Consejo Nacional de Investigaciones 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: Mitnik, Dario Marcelo. Consejo Nacional de Investigaciones 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; ArgentinaEDP Sciences2021-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/182597Peralta, Juan Ignacio; Vieytes, Mariela Cristina; Mendez, Marta Patricia Alejandra; Mitnik, Dario Marcelo; Modeling the Mg I from the NUV to MIR. I. The solar case; EDP Sciences; Astronomy and Astrophysics; 657; 11-2021; 1-140004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2022/01/aa41973-21/aa41973-21.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202141973info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2110.02992info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:42:48Zoai:ri.conicet.gov.ar:11336/182597instacron: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 09:42:49.014CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Modeling the Mg I from the NUV to MIR. I. The solar case |
title |
Modeling the Mg I from the NUV to MIR. I. The solar case |
spellingShingle |
Modeling the Mg I from the NUV to MIR. I. The solar case Peralta, Juan Ignacio ATOMIC DATA LINE: FORMATION LINE: PROFILES SUN: ATMOSPHERE SUN: INFRARED |
title_short |
Modeling the Mg I from the NUV to MIR. I. The solar case |
title_full |
Modeling the Mg I from the NUV to MIR. I. The solar case |
title_fullStr |
Modeling the Mg I from the NUV to MIR. I. The solar case |
title_full_unstemmed |
Modeling the Mg I from the NUV to MIR. I. The solar case |
title_sort |
Modeling the Mg I from the NUV to MIR. I. The solar case |
dc.creator.none.fl_str_mv |
Peralta, Juan Ignacio Vieytes, Mariela Cristina Mendez, Marta Patricia Alejandra Mitnik, Dario Marcelo |
author |
Peralta, Juan Ignacio |
author_facet |
Peralta, Juan Ignacio Vieytes, Mariela Cristina Mendez, Marta Patricia Alejandra Mitnik, Dario Marcelo |
author_role |
author |
author2 |
Vieytes, Mariela Cristina Mendez, Marta Patricia Alejandra Mitnik, Dario Marcelo |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
ATOMIC DATA LINE: FORMATION LINE: PROFILES SUN: ATMOSPHERE SUN: INFRARED |
topic |
ATOMIC DATA LINE: FORMATION LINE: PROFILES SUN: ATMOSPHERE SUN: INFRARED |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Context. Semi-empirical models of the solar atmosphere are used to study the radiative environment of any planet in our Solar System. There is a need for reliable atomic data for neutral atoms and ions in the atmosphere to obtain improved calculated spectra. Atomic parameters are crucial to computing the correct population of elements through the whole stellar atmosphere. Although there is very good agreement between the observed and calculated spectra for the Sun, there is still a mismatch in several spectral ranges due to the lack of atomic data and the inaccuracies thereof, particularly for neutrals such as Mga» I. Aims. To represent many spectral lines of Mga» I from the near-ultraviolet to the mid-infrared correctly, it is necessary to add and update the atomic data involved in the atomic processes that drive their formation. Methods. The improvements made to the Mga» I atomic model are as follows: i) 127 strong lines, including their broadening data, were added. ii) To obtain these new lines, we increased the number of energy levels from 26 to 85. iii) Photoionization cross-section parameters were added and updated. iv) Effective collision strength (I' ij ) parameters were updated for the first 25 levels using the existing data from the convergent close-coupling calculations. One of the most significant changes in our model is given by the new I' ij parameters for transitions involving levels between 26 and 54, which were computed with a multiconfiguration Breit-Pauli distorted-wave (DW) method. For transitions involving superlevels, we calculated the I' ij parameters with the usual semi-empirical formulas. Results. More than 100 transitions were added to our calculations, increasing our capability of reproducing important features observed in the solar spectra. We found a remarkable improvement in matching the solar spectra for wavelengths higher than 30 000 Å when our new DW I' ij data were used in the model. Fil: Peralta, Juan Ignacio. Universidad Nacional de Tres de Febrero; Argentina. Consejo Nacional de Investigaciones 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: Vieytes, Mariela Cristina. Universidad Nacional de Tres de Febrero; Argentina. Consejo Nacional de Investigaciones 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: Mendez, Marta Patricia Alejandra. Consejo Nacional de Investigaciones 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: Mitnik, Dario Marcelo. Consejo Nacional de Investigaciones 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 |
description |
Context. Semi-empirical models of the solar atmosphere are used to study the radiative environment of any planet in our Solar System. There is a need for reliable atomic data for neutral atoms and ions in the atmosphere to obtain improved calculated spectra. Atomic parameters are crucial to computing the correct population of elements through the whole stellar atmosphere. Although there is very good agreement between the observed and calculated spectra for the Sun, there is still a mismatch in several spectral ranges due to the lack of atomic data and the inaccuracies thereof, particularly for neutrals such as Mga» I. Aims. To represent many spectral lines of Mga» I from the near-ultraviolet to the mid-infrared correctly, it is necessary to add and update the atomic data involved in the atomic processes that drive their formation. Methods. The improvements made to the Mga» I atomic model are as follows: i) 127 strong lines, including their broadening data, were added. ii) To obtain these new lines, we increased the number of energy levels from 26 to 85. iii) Photoionization cross-section parameters were added and updated. iv) Effective collision strength (I' ij ) parameters were updated for the first 25 levels using the existing data from the convergent close-coupling calculations. One of the most significant changes in our model is given by the new I' ij parameters for transitions involving levels between 26 and 54, which were computed with a multiconfiguration Breit-Pauli distorted-wave (DW) method. For transitions involving superlevels, we calculated the I' ij parameters with the usual semi-empirical formulas. Results. More than 100 transitions were added to our calculations, increasing our capability of reproducing important features observed in the solar spectra. We found a remarkable improvement in matching the solar spectra for wavelengths higher than 30 000 Å when our new DW I' ij data were used in the model. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-11 |
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/11336/182597 Peralta, Juan Ignacio; Vieytes, Mariela Cristina; Mendez, Marta Patricia Alejandra; Mitnik, Dario Marcelo; Modeling the Mg I from the NUV to MIR. I. The solar case; EDP Sciences; Astronomy and Astrophysics; 657; 11-2021; 1-14 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/182597 |
identifier_str_mv |
Peralta, Juan Ignacio; Vieytes, Mariela Cristina; Mendez, Marta Patricia Alejandra; Mitnik, Dario Marcelo; Modeling the Mg I from the NUV to MIR. I. The solar case; EDP Sciences; Astronomy and Astrophysics; 657; 11-2021; 1-14 0004-6361 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2022/01/aa41973-21/aa41973-21.html info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202141973 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2110.02992 |
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/ |
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application/pdf application/pdf application/pdf |
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EDP Sciences |
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EDP Sciences |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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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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