Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b

Autores
Villarreal D'angelo, Carolina Susana; Esquivel Salazar, José Alejandro; Schneiter, Ernesto Matías; Sgró, Mario Agustín
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Lyman a observations during an exoplanet transit have proved to be very useful to study the interaction between the stellar wind and the planetary atmosphere. They have been extensively used to constrain planetary system parameters that are not directly observed, such as the planetary mass-loss rate. In this way, Ly α observations can be a powerful tool to infer the existence of a planetarymagnetic field, since it is expected that the latterwill affect the escaping planetary material. To explore the effect that magnetic fields have on the Ly α absorption of HD 209458b, we run a set of 3D MHD simulations including dipolar magnetic fields for the planet and the star. We assume values for the surface magnetic field at the poles of the planet in the range of [0-5] G, and from 1 to 5 G at the poles of the star. Our models also include collisional and photo-ionization, radiative recombination, and an approximation for the radiation pressure. Our results show that the magnetic field of the planet and the star change the shape of the Ly α absorption profile, since it controls the extent of the planetary magnetosphere and the amount of neutralmaterial inside it. Themodel that best reproduces the absorption observed in HD 209458b (with canonical values for the stellar wind parameters) corresponds to a dipole planetary field of ≲ 1 G at the poles.
Fil: Villarreal D'angelo, Carolina Susana. University of St. Andrews; Reino Unido
Fil: Esquivel Salazar, José Alejandro. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Schneiter, Ernesto Matías. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Sgró, Mario Agustín. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Materia
MHD-METHODS: NUMERICAL
PLANET-STAR INTERACTIONS
PLANETS AND SATELLITES: GENERAL
PLANETS AND SATELLITES: INDIVIDUAL: HD 209458B
STARS: WINDS, OUTFLOWS
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:11336/86936
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/86936
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Magnetized winds and their influence in the escaping upper atmosphere of HD 209458bVillarreal D'angelo, Carolina SusanaEsquivel Salazar, José AlejandroSchneiter, Ernesto MatíasSgró, Mario AgustínMHD-METHODS: NUMERICALPLANET-STAR INTERACTIONSPLANETS AND SATELLITES: GENERALPLANETS AND SATELLITES: INDIVIDUAL: HD 209458BSTARS: WINDS, OUTFLOWShttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Lyman a observations during an exoplanet transit have proved to be very useful to study the interaction between the stellar wind and the planetary atmosphere. They have been extensively used to constrain planetary system parameters that are not directly observed, such as the planetary mass-loss rate. In this way, Ly α observations can be a powerful tool to infer the existence of a planetarymagnetic field, since it is expected that the latterwill affect the escaping planetary material. To explore the effect that magnetic fields have on the Ly α absorption of HD 209458b, we run a set of 3D MHD simulations including dipolar magnetic fields for the planet and the star. We assume values for the surface magnetic field at the poles of the planet in the range of [0-5] G, and from 1 to 5 G at the poles of the star. Our models also include collisional and photo-ionization, radiative recombination, and an approximation for the radiation pressure. Our results show that the magnetic field of the planet and the star change the shape of the Ly α absorption profile, since it controls the extent of the planetary magnetosphere and the amount of neutralmaterial inside it. Themodel that best reproduces the absorption observed in HD 209458b (with canonical values for the stellar wind parameters) corresponds to a dipole planetary field of ≲ 1 G at the poles.Fil: Villarreal D'angelo, Carolina Susana. University of St. Andrews; Reino UnidoFil: Esquivel Salazar, José Alejandro. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoFil: Schneiter, Ernesto Matías. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Sgró, Mario Agustín. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaWiley Blackwell Publishing, Inc2018-09info: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/11336/86936Villarreal D'angelo, Carolina Susana; Esquivel Salazar, José Alejandro; Schneiter, Ernesto Matías; Sgró, Mario Agustín; Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 3; 9-2018; 3115-31250035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/479/3/3115/5035846info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1544info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:59:58Zoai:ri.conicet.gov.ar:11336/86936instacron: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 09:59:58.606CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
title Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
spellingShingle Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
Villarreal D'angelo, Carolina Susana
MHD-METHODS: NUMERICAL
PLANET-STAR INTERACTIONS
PLANETS AND SATELLITES: GENERAL
PLANETS AND SATELLITES: INDIVIDUAL: HD 209458B
STARS: WINDS, OUTFLOWS
title_short Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
title_full Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
title_fullStr Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
title_full_unstemmed Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
title_sort Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b
dc.creator.none.fl_str_mv Villarreal D'angelo, Carolina Susana
Esquivel Salazar, José Alejandro
Schneiter, Ernesto Matías
Sgró, Mario Agustín
author Villarreal D'angelo, Carolina Susana
author_facet Villarreal D'angelo, Carolina Susana
Esquivel Salazar, José Alejandro
Schneiter, Ernesto Matías
Sgró, Mario Agustín
author_role author
author2 Esquivel Salazar, José Alejandro
Schneiter, Ernesto Matías
Sgró, Mario Agustín
author2_role author
author
author
dc.subject.none.fl_str_mv MHD-METHODS: NUMERICAL
PLANET-STAR INTERACTIONS
PLANETS AND SATELLITES: GENERAL
PLANETS AND SATELLITES: INDIVIDUAL: HD 209458B
STARS: WINDS, OUTFLOWS
topic MHD-METHODS: NUMERICAL
PLANET-STAR INTERACTIONS
PLANETS AND SATELLITES: GENERAL
PLANETS AND SATELLITES: INDIVIDUAL: HD 209458B
STARS: WINDS, OUTFLOWS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.7
https://purl.org/becyt/ford/1
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Lyman a observations during an exoplanet transit have proved to be very useful to study the interaction between the stellar wind and the planetary atmosphere. They have been extensively used to constrain planetary system parameters that are not directly observed, such as the planetary mass-loss rate. In this way, Ly α observations can be a powerful tool to infer the existence of a planetarymagnetic field, since it is expected that the latterwill affect the escaping planetary material. To explore the effect that magnetic fields have on the Ly α absorption of HD 209458b, we run a set of 3D MHD simulations including dipolar magnetic fields for the planet and the star. We assume values for the surface magnetic field at the poles of the planet in the range of [0-5] G, and from 1 to 5 G at the poles of the star. Our models also include collisional and photo-ionization, radiative recombination, and an approximation for the radiation pressure. Our results show that the magnetic field of the planet and the star change the shape of the Ly α absorption profile, since it controls the extent of the planetary magnetosphere and the amount of neutralmaterial inside it. Themodel that best reproduces the absorption observed in HD 209458b (with canonical values for the stellar wind parameters) corresponds to a dipole planetary field of ≲ 1 G at the poles.
Fil: Villarreal D'angelo, Carolina Susana. University of St. Andrews; Reino Unido
Fil: Esquivel Salazar, José Alejandro. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Schneiter, Ernesto Matías. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Sgró, Mario Agustín. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
description Lyman a observations during an exoplanet transit have proved to be very useful to study the interaction between the stellar wind and the planetary atmosphere. They have been extensively used to constrain planetary system parameters that are not directly observed, such as the planetary mass-loss rate. In this way, Ly α observations can be a powerful tool to infer the existence of a planetarymagnetic field, since it is expected that the latterwill affect the escaping planetary material. To explore the effect that magnetic fields have on the Ly α absorption of HD 209458b, we run a set of 3D MHD simulations including dipolar magnetic fields for the planet and the star. We assume values for the surface magnetic field at the poles of the planet in the range of [0-5] G, and from 1 to 5 G at the poles of the star. Our models also include collisional and photo-ionization, radiative recombination, and an approximation for the radiation pressure. Our results show that the magnetic field of the planet and the star change the shape of the Ly α absorption profile, since it controls the extent of the planetary magnetosphere and the amount of neutralmaterial inside it. Themodel that best reproduces the absorption observed in HD 209458b (with canonical values for the stellar wind parameters) corresponds to a dipole planetary field of ≲ 1 G at the poles.
publishDate 2018
dc.date.none.fl_str_mv 2018-09
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/11336/86936
Villarreal D'angelo, Carolina Susana; Esquivel Salazar, José Alejandro; Schneiter, Ernesto Matías; Sgró, Mario Agustín; Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 3; 9-2018; 3115-3125
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/86936
identifier_str_mv Villarreal D'angelo, Carolina Susana; Esquivel Salazar, José Alejandro; Schneiter, Ernesto Matías; Sgró, Mario Agustín; Magnetized winds and their influence in the escaping upper atmosphere of HD 209458b; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 3; 9-2018; 3115-3125
0035-8711
1365-2966
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://academic.oup.com/mnras/article/479/3/3115/5035846
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1544
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
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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
_version_ 1844613776329932800
score 13.070432

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