On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study

Autores
Villarreal D'angelo, Carolina Susana; Schneiter, Ernesto Matías; Costa, Andrea; Velázquez, P.; Raga, A.; Esquivel, A.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present a 3D hydrodynamic study of the effects that different stellar wind conditions and planetary wind structures have on the calculated Lyα absorptions produced by a cometary tail during transit. We concentrate, as a case study, on the known HD 209458b case. Initially, we assume a broad range of possible planetary mass-loss rate values: M˙ p = [1−7] × 1010 g s−1. Then, by comparing the observational Lyα absorption with the numerically derived ones, we could constrain the M˙ p values within the given range. We find that the planetary massloss rate does not change dramatically for large changes in stellar wind speeds ∼[250– 800] km s−1 and temperature ∼[3–7] × 106 K while keeping fixed the stellar mass-loss rate (M˙ = 9.0 × 10−14 M yr−1). The M˙ p range found is ∼ [3−5] × 1010 g s−1, depending upon the efficiency of the stellar wind to transport heat (polytropic index ∼ [1.01–1.13]), leading to different stellar wind speeds. Several models with anisotropic evaporation profiles for the planetary escaping atmosphere were carried out, showing that both, the escape through polar regions, resembling the emission associated with reconnection processes, and through the night side, produced by a strong stellar wind that compresses the planetary atmosphere and inhibits its escape from the day hemisphere yields larger absorptions than an isotropic planetary wind.
Fil: Villarreal D'angelo, Carolina Susana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Schneiter, Ernesto Matías. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Costa, Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Velázquez, P.. Universidad Nacional Autónoma de México; México
Fil: Raga, A.. Universidad Nacional Autónoma de México; México
Fil: Esquivel, A.. Universidad Nacional Autónoma de México; México
Materia
Exoplanet
HD
Plasma
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:11336/26372
Acceder
id CONICETDig_35c705eb2641daf5e8dbf9aa45acdec1
oai_identifier_str oai:ri.conicet.gov.ar:11336/26372
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case studyVillarreal D'angelo, Carolina SusanaSchneiter, Ernesto MatíasCosta, AndreaVelázquez, P.Raga, A.Esquivel, A.ExoplanetHDPlasmahttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a 3D hydrodynamic study of the effects that different stellar wind conditions and planetary wind structures have on the calculated Lyα absorptions produced by a cometary tail during transit. We concentrate, as a case study, on the known HD 209458b case. Initially, we assume a broad range of possible planetary mass-loss rate values: M˙ p = [1−7] × 1010 g s−1. Then, by comparing the observational Lyα absorption with the numerically derived ones, we could constrain the M˙ p values within the given range. We find that the planetary massloss rate does not change dramatically for large changes in stellar wind speeds ∼[250– 800] km s−1 and temperature ∼[3–7] × 106 K while keeping fixed the stellar mass-loss rate (M˙ = 9.0 × 10−14 M yr−1). The M˙ p range found is ∼ [3−5] × 1010 g s−1, depending upon the efficiency of the stellar wind to transport heat (polytropic index ∼ [1.01–1.13]), leading to different stellar wind speeds. Several models with anisotropic evaporation profiles for the planetary escaping atmosphere were carried out, showing that both, the escape through polar regions, resembling the emission associated with reconnection processes, and through the night side, produced by a strong stellar wind that compresses the planetary atmosphere and inhibits its escape from the day hemisphere yields larger absorptions than an isotropic planetary wind.Fil: Villarreal D'angelo, Carolina Susana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Schneiter, Ernesto Matías. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Costa, Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Velázquez, P.. Universidad Nacional Autónoma de México; MéxicoFil: Raga, A.. Universidad Nacional Autónoma de México; MéxicoFil: Esquivel, A.. Universidad Nacional Autónoma de México; MéxicoOxford University Press2013-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/26372Villarreal D'angelo, Carolina Susana; Schneiter, Ernesto Matías; Costa, Andrea; Velázquez, P.; Raga, A.; et al.; On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 438; 2; 12-2013; 1654-16620035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stt2303info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stt2303info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1312.6126info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:15:15Zoai:ri.conicet.gov.ar:11336/26372instacron: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:34982025-10-22 11:15:15.684CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
title On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
spellingShingle On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
Villarreal D'angelo, Carolina Susana
Exoplanet
HD
Plasma
title_short On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
title_full On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
title_fullStr On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
title_full_unstemmed On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
title_sort On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
dc.creator.none.fl_str_mv Villarreal D'angelo, Carolina Susana
Schneiter, Ernesto Matías
Costa, Andrea
Velázquez, P.
Raga, A.
Esquivel, A.
author Villarreal D'angelo, Carolina Susana
author_facet Villarreal D'angelo, Carolina Susana
Schneiter, Ernesto Matías
Costa, Andrea
Velázquez, P.
Raga, A.
Esquivel, A.
author_role author
author2 Schneiter, Ernesto Matías
Costa, Andrea
Velázquez, P.
Raga, A.
Esquivel, A.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Exoplanet
HD
Plasma
topic Exoplanet
HD
Plasma
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 present a 3D hydrodynamic study of the effects that different stellar wind conditions and planetary wind structures have on the calculated Lyα absorptions produced by a cometary tail during transit. We concentrate, as a case study, on the known HD 209458b case. Initially, we assume a broad range of possible planetary mass-loss rate values: M˙ p = [1−7] × 1010 g s−1. Then, by comparing the observational Lyα absorption with the numerically derived ones, we could constrain the M˙ p values within the given range. We find that the planetary massloss rate does not change dramatically for large changes in stellar wind speeds ∼[250– 800] km s−1 and temperature ∼[3–7] × 106 K while keeping fixed the stellar mass-loss rate (M˙ = 9.0 × 10−14 M yr−1). The M˙ p range found is ∼ [3−5] × 1010 g s−1, depending upon the efficiency of the stellar wind to transport heat (polytropic index ∼ [1.01–1.13]), leading to different stellar wind speeds. Several models with anisotropic evaporation profiles for the planetary escaping atmosphere were carried out, showing that both, the escape through polar regions, resembling the emission associated with reconnection processes, and through the night side, produced by a strong stellar wind that compresses the planetary atmosphere and inhibits its escape from the day hemisphere yields larger absorptions than an isotropic planetary wind.
Fil: Villarreal D'angelo, Carolina Susana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Schneiter, Ernesto Matías. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Costa, Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Velázquez, P.. Universidad Nacional Autónoma de México; México
Fil: Raga, A.. Universidad Nacional Autónoma de México; México
Fil: Esquivel, A.. Universidad Nacional Autónoma de México; México
description We present a 3D hydrodynamic study of the effects that different stellar wind conditions and planetary wind structures have on the calculated Lyα absorptions produced by a cometary tail during transit. We concentrate, as a case study, on the known HD 209458b case. Initially, we assume a broad range of possible planetary mass-loss rate values: M˙ p = [1−7] × 1010 g s−1. Then, by comparing the observational Lyα absorption with the numerically derived ones, we could constrain the M˙ p values within the given range. We find that the planetary massloss rate does not change dramatically for large changes in stellar wind speeds ∼[250– 800] km s−1 and temperature ∼[3–7] × 106 K while keeping fixed the stellar mass-loss rate (M˙ = 9.0 × 10−14 M yr−1). The M˙ p range found is ∼ [3−5] × 1010 g s−1, depending upon the efficiency of the stellar wind to transport heat (polytropic index ∼ [1.01–1.13]), leading to different stellar wind speeds. Several models with anisotropic evaporation profiles for the planetary escaping atmosphere were carried out, showing that both, the escape through polar regions, resembling the emission associated with reconnection processes, and through the night side, produced by a strong stellar wind that compresses the planetary atmosphere and inhibits its escape from the day hemisphere yields larger absorptions than an isotropic planetary wind.
publishDate 2013
dc.date.none.fl_str_mv 2013-12
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/11336/26372
Villarreal D'angelo, Carolina Susana; Schneiter, Ernesto Matías; Costa, Andrea; Velázquez, P.; Raga, A.; et al.; On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 438; 2; 12-2013; 1654-1662
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/26372
identifier_str_mv Villarreal D'angelo, Carolina Susana; Schneiter, Ernesto Matías; Costa, Andrea; Velázquez, P.; Raga, A.; et al.; On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 438; 2; 12-2013; 1654-1662
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stt2303
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stt2303
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1312.6126
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
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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_ 1846781584376594432
score 12.982451

Publicaciones similares