The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b
- Autores
- Hazra, Gopal; Vidotto, Aline A.; Carolan, Stephen; Villarreal D'angelo, Carolina Susana; Manchester, Ward
- Año de publicación
- 2022
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- High-energy stellar irradiation can photoevaporate planetary atmospheres, which can be observed in spectroscopic transits of hydrogen lines. For the exoplanet HD189733b, multiple observations in the Ly α line have shown that atmospheric evaporation is variable, going from undetected to enhanced evaporation in a 1.5-yr interval. Coincidentally or not, when HD189733b was observed to be evaporating, a stellar flare had just occurred 8 h prior to the observation. This led to the question of whether this temporal variation in evaporation occurred due to the flare, an unseen associated coronal mass ejection (CME), or even the simultaneous effect of both. In this work, we investigate the impact of flares (radiation), winds, and CMEs (particles) on the atmosphere of HD189733b using three-dimensional radiation hydrodynamic simulations that self-consistently include stellar photon heating. We study four cases: first, the quiescent phase including stellar wind; secondly, a flare; thirdly, a CME; and fourthly, a flare that is followed by a CME. Compared to the quiescent case, we find that the flare alone increases the evaporation rate by only 25 per cent, while the CME leads to a factor of 4 increments. We calculate Ly α synthetic transits and find that the flare alone cannot explain the observed high blueshifted velocities seen in the Ly α. The CME, however, leads to an increase in the velocity of escaping atmospheres, enhancing the blueshifted transit depth. While the effects of CMEs show a promising potential, our models are not able to fully explain the blueshifted transit depths, indicating that they might require additional physical mechanisms.
Fil: Hazra, Gopal. Leiden University; Países Bajos
Fil: Vidotto, Aline A.. Leiden University; Países Bajos
Fil: Carolan, Stephen. Trinity College Dublin; Irlanda
Fil: Villarreal D'angelo, Carolina Susana. 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: Manchester, Ward. University of Michigan; Estados Unidos - Materia
-
PLANETS AND SATELLITES: ATMOSPHERE
PLANET–STAR INTERACTIONS
STARS: CORONAL MASS EJECTIONS
STARS: FLARES
STARS: HD189733A - 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:11336/216390
Ver los metadatos del registro completo
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spelling |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733bHazra, GopalVidotto, Aline A.Carolan, StephenVillarreal D'angelo, Carolina SusanaManchester, WardPLANETS AND SATELLITES: ATMOSPHEREPLANET–STAR INTERACTIONSSTARS: CORONAL MASS EJECTIONSSTARS: FLARESSTARS: HD189733Ahttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1High-energy stellar irradiation can photoevaporate planetary atmospheres, which can be observed in spectroscopic transits of hydrogen lines. For the exoplanet HD189733b, multiple observations in the Ly α line have shown that atmospheric evaporation is variable, going from undetected to enhanced evaporation in a 1.5-yr interval. Coincidentally or not, when HD189733b was observed to be evaporating, a stellar flare had just occurred 8 h prior to the observation. This led to the question of whether this temporal variation in evaporation occurred due to the flare, an unseen associated coronal mass ejection (CME), or even the simultaneous effect of both. In this work, we investigate the impact of flares (radiation), winds, and CMEs (particles) on the atmosphere of HD189733b using three-dimensional radiation hydrodynamic simulations that self-consistently include stellar photon heating. We study four cases: first, the quiescent phase including stellar wind; secondly, a flare; thirdly, a CME; and fourthly, a flare that is followed by a CME. Compared to the quiescent case, we find that the flare alone increases the evaporation rate by only 25 per cent, while the CME leads to a factor of 4 increments. We calculate Ly α synthetic transits and find that the flare alone cannot explain the observed high blueshifted velocities seen in the Ly α. The CME, however, leads to an increase in the velocity of escaping atmospheres, enhancing the blueshifted transit depth. While the effects of CMEs show a promising potential, our models are not able to fully explain the blueshifted transit depths, indicating that they might require additional physical mechanisms.Fil: Hazra, Gopal. Leiden University; Países BajosFil: Vidotto, Aline A.. Leiden University; Países BajosFil: Carolan, Stephen. Trinity College Dublin; IrlandaFil: Villarreal D'angelo, Carolina Susana. 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: Manchester, Ward. University of Michigan; Estados UnidosWiley Blackwell Publishing, Inc2022-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/216390Hazra, Gopal; Vidotto, Aline A.; Carolan, Stephen; Villarreal D'angelo, Carolina Susana; Manchester, Ward; The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 509; 4; 2-2022; 5858-58710035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stab3271info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:10:50Zoai:ri.conicet.gov.ar:11336/216390instacron: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 10:10:50.388CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
title |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
spellingShingle |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b Hazra, Gopal PLANETS AND SATELLITES: ATMOSPHERE PLANET–STAR INTERACTIONS STARS: CORONAL MASS EJECTIONS STARS: FLARES STARS: HD189733A |
title_short |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
title_full |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
title_fullStr |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
title_full_unstemmed |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
title_sort |
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b |
dc.creator.none.fl_str_mv |
Hazra, Gopal Vidotto, Aline A. Carolan, Stephen Villarreal D'angelo, Carolina Susana Manchester, Ward |
author |
Hazra, Gopal |
author_facet |
Hazra, Gopal Vidotto, Aline A. Carolan, Stephen Villarreal D'angelo, Carolina Susana Manchester, Ward |
author_role |
author |
author2 |
Vidotto, Aline A. Carolan, Stephen Villarreal D'angelo, Carolina Susana Manchester, Ward |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
PLANETS AND SATELLITES: ATMOSPHERE PLANET–STAR INTERACTIONS STARS: CORONAL MASS EJECTIONS STARS: FLARES STARS: HD189733A |
topic |
PLANETS AND SATELLITES: ATMOSPHERE PLANET–STAR INTERACTIONS STARS: CORONAL MASS EJECTIONS STARS: FLARES STARS: HD189733A |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.7 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
High-energy stellar irradiation can photoevaporate planetary atmospheres, which can be observed in spectroscopic transits of hydrogen lines. For the exoplanet HD189733b, multiple observations in the Ly α line have shown that atmospheric evaporation is variable, going from undetected to enhanced evaporation in a 1.5-yr interval. Coincidentally or not, when HD189733b was observed to be evaporating, a stellar flare had just occurred 8 h prior to the observation. This led to the question of whether this temporal variation in evaporation occurred due to the flare, an unseen associated coronal mass ejection (CME), or even the simultaneous effect of both. In this work, we investigate the impact of flares (radiation), winds, and CMEs (particles) on the atmosphere of HD189733b using three-dimensional radiation hydrodynamic simulations that self-consistently include stellar photon heating. We study four cases: first, the quiescent phase including stellar wind; secondly, a flare; thirdly, a CME; and fourthly, a flare that is followed by a CME. Compared to the quiescent case, we find that the flare alone increases the evaporation rate by only 25 per cent, while the CME leads to a factor of 4 increments. We calculate Ly α synthetic transits and find that the flare alone cannot explain the observed high blueshifted velocities seen in the Ly α. The CME, however, leads to an increase in the velocity of escaping atmospheres, enhancing the blueshifted transit depth. While the effects of CMEs show a promising potential, our models are not able to fully explain the blueshifted transit depths, indicating that they might require additional physical mechanisms. Fil: Hazra, Gopal. Leiden University; Países Bajos Fil: Vidotto, Aline A.. Leiden University; Países Bajos Fil: Carolan, Stephen. Trinity College Dublin; Irlanda Fil: Villarreal D'angelo, Carolina Susana. 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: Manchester, Ward. University of Michigan; Estados Unidos |
description |
High-energy stellar irradiation can photoevaporate planetary atmospheres, which can be observed in spectroscopic transits of hydrogen lines. For the exoplanet HD189733b, multiple observations in the Ly α line have shown that atmospheric evaporation is variable, going from undetected to enhanced evaporation in a 1.5-yr interval. Coincidentally or not, when HD189733b was observed to be evaporating, a stellar flare had just occurred 8 h prior to the observation. This led to the question of whether this temporal variation in evaporation occurred due to the flare, an unseen associated coronal mass ejection (CME), or even the simultaneous effect of both. In this work, we investigate the impact of flares (radiation), winds, and CMEs (particles) on the atmosphere of HD189733b using three-dimensional radiation hydrodynamic simulations that self-consistently include stellar photon heating. We study four cases: first, the quiescent phase including stellar wind; secondly, a flare; thirdly, a CME; and fourthly, a flare that is followed by a CME. Compared to the quiescent case, we find that the flare alone increases the evaporation rate by only 25 per cent, while the CME leads to a factor of 4 increments. We calculate Ly α synthetic transits and find that the flare alone cannot explain the observed high blueshifted velocities seen in the Ly α. The CME, however, leads to an increase in the velocity of escaping atmospheres, enhancing the blueshifted transit depth. While the effects of CMEs show a promising potential, our models are not able to fully explain the blueshifted transit depths, indicating that they might require additional physical mechanisms. |
publishDate |
2022 |
dc.date.none.fl_str_mv |
2022-02 |
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/11336/216390 Hazra, Gopal; Vidotto, Aline A.; Carolan, Stephen; Villarreal D'angelo, Carolina Susana; Manchester, Ward; The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 509; 4; 2-2022; 5858-5871 0035-8711 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/216390 |
identifier_str_mv |
Hazra, Gopal; Vidotto, Aline A.; Carolan, Stephen; Villarreal D'angelo, Carolina Susana; Manchester, Ward; The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 509; 4; 2-2022; 5858-5871 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/stab3271 |
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 |
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 |
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1844614001358536704 |
score |
13.070432 |