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dc.contributor.author
Hazra, Gopal
dc.contributor.author
Vidotto, Aline A.
dc.contributor.author
Carolan, Stephen
dc.contributor.author
Villarreal D'angelo, Carolina Susana
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dc.contributor.author
Manchester, Ward
dc.date.available
2023-10-30T14:19:53Z
dc.date.issued
2022-02
dc.identifier.citation
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
dc.identifier.issn
0035-8711
dc.identifier.uri
http://hdl.handle.net/11336/216390
dc.description.abstract
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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Wiley Blackwell Publishing, Inc
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
PLANETS AND SATELLITES: ATMOSPHERE
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PLANET–STAR INTERACTIONS
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STARS: CORONAL MASS EJECTIONS
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STARS: FLARES
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STARS: HD189733A
dc.subject.classification
Otras Ciencias Naturales y Exactas
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dc.subject.classification
Otras Ciencias Naturales y Exactas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2023-10-26T15:11:31Z
dc.journal.volume
509
dc.journal.number
4
dc.journal.pagination
5858-5871
dc.journal.pais
Reino Unido
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dc.journal.ciudad
Londres
dc.description.fil
Fil: Hazra, Gopal. Leiden University; Países Bajos
dc.description.fil
Fil: Vidotto, Aline A.. Leiden University; Países Bajos
dc.description.fil
Fil: Carolan, Stephen. Trinity College Dublin; Irlanda
dc.description.fil
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
dc.description.fil
Fil: Manchester, Ward. University of Michigan; Estados Unidos
dc.journal.title
Monthly Notices of the Royal Astronomical Society
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1093/mnras/stab3271
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