Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832

Autores
Fontenla, J. M.; Linsky, J. L.; Witbrod, J.; France, K.; Buccino, Andrea Paola; Mauas, Pablo Jacobo David; Vieytes, Mariela Cristina; Walkowicz, L.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Stellar radiation from X-rays to the visible provides the energy thatcontrols the photochemistry and mass loss from exoplanet atmospheres.The important extreme ultraviolet (EUV) region (10-91.2 nm) isinaccessible and should be computed from a reliable stellar model. It isessential to understand the formation regions and physical processesresponsible for the various stellar emission features to predict how thespectral energy distribution varies with age and activity levels. Wecompute a state-of-the-art semi-empirical atmospheric model and theemergent high-resolution synthetic spectrum of the moderately active M2V star GJ 832 as the first of a series of models for stars withdifferent activity levels. We construct a one-dimensional simple modelfor the physical structure of the star?s chromosphere,chromosphere-corona transition region, and corona using non-LTEradiative transfer techniques and many molecular lines. The synthesizedspectrum for this model fits the continuum and lines across theUV-to-optical spectrum. Particular emphasis is given to the emissionlines at wavelengths that are shorter than 300 nm observed with theHubble Space Telescope, which have important effects on thephotochemistry of the exoplanet atmospheres. The FUV line ratiosindicate that the transition region of GJ 832 is more biased to hottermaterial than that of the quiet Sun. The excellent agreement of ourcomputed EUV luminosity with that obtained by two other techniquesindicates that our model predicts reliable EUV emission from GJ 832. Wefind that the unobserved EUV flux of GJ 832, which heats the outeratmospheres of exoplanets and drives their mass loss, is comparable tothe active Sun.
Fil: Fontenla, J. M.. State University Of Colorado Boulder; Estados Unidos
Fil: Linsky, J. L.. State University Of Colorado Boulder; Estados Unidos
Fil: Witbrod, J.. State University Of Colorado Boulder; Estados Unidos
Fil: France, K.. State University Of Colorado Boulder; Estados Unidos
Fil: Buccino, Andrea Paola. 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: Mauas, Pablo Jacobo David. 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: Vieytes, Mariela Cristina. 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: Walkowicz, L.. The Adler Planetarium; Estados Unidos
Materia
planetstar interactions
ultraviolet: stars
stars: late-type
stars: individual: GJ 832
stars: coronae
stars: chromospheres
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:11336/21732
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/21732
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832Fontenla, J. M.Linsky, J. L.Witbrod, J.France, K.Buccino, Andrea PaolaMauas, Pablo Jacobo DavidVieytes, Mariela CristinaWalkowicz, L.planetstar interactionsultraviolet: starsstars: late-typestars: individual: GJ 832stars: coronaestars: chromosphereshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Stellar radiation from X-rays to the visible provides the energy thatcontrols the photochemistry and mass loss from exoplanet atmospheres.The important extreme ultraviolet (EUV) region (10-91.2 nm) isinaccessible and should be computed from a reliable stellar model. It isessential to understand the formation regions and physical processesresponsible for the various stellar emission features to predict how thespectral energy distribution varies with age and activity levels. Wecompute a state-of-the-art semi-empirical atmospheric model and theemergent high-resolution synthetic spectrum of the moderately active M2V star GJ 832 as the first of a series of models for stars withdifferent activity levels. We construct a one-dimensional simple modelfor the physical structure of the star?s chromosphere,chromosphere-corona transition region, and corona using non-LTEradiative transfer techniques and many molecular lines. The synthesizedspectrum for this model fits the continuum and lines across theUV-to-optical spectrum. Particular emphasis is given to the emissionlines at wavelengths that are shorter than 300 nm observed with theHubble Space Telescope, which have important effects on thephotochemistry of the exoplanet atmospheres. The FUV line ratiosindicate that the transition region of GJ 832 is more biased to hottermaterial than that of the quiet Sun. The excellent agreement of ourcomputed EUV luminosity with that obtained by two other techniquesindicates that our model predicts reliable EUV emission from GJ 832. Wefind that the unobserved EUV flux of GJ 832, which heats the outeratmospheres of exoplanets and drives their mass loss, is comparable tothe active Sun.Fil: Fontenla, J. M.. State University Of Colorado Boulder; Estados UnidosFil: Linsky, J. L.. State University Of Colorado Boulder; Estados UnidosFil: Witbrod, J.. State University Of Colorado Boulder; Estados UnidosFil: France, K.. State University Of Colorado Boulder; Estados UnidosFil: Buccino, Andrea Paola. 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: Mauas, Pablo Jacobo David. 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: Vieytes, Mariela Cristina. 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: Walkowicz, L.. The Adler Planetarium; Estados UnidosIOP Publishing2016-10info: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/11336/21732Fontenla, J. M.; Linsky, J. L.; Witbrod, J.; France, K.; Buccino, Andrea Paola; et al.; Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832; IOP Publishing; Astrophysical Journal; 830; 2; 10-2016; 154,1-180004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/0004-637X/830/2/154info:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/830/2/154info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1608.00934info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:46:28Zoai:ri.conicet.gov.ar:11336/21732instacron: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 09:46:28.894CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
title Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
spellingShingle Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
Fontenla, J. M.
planetstar interactions
ultraviolet: stars
stars: late-type
stars: individual: GJ 832
stars: coronae
stars: chromospheres
title_short Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
title_full Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
title_fullStr Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
title_full_unstemmed Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
title_sort Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832
dc.creator.none.fl_str_mv Fontenla, J. M.
Linsky, J. L.
Witbrod, J.
France, K.
Buccino, Andrea Paola
Mauas, Pablo Jacobo David
Vieytes, Mariela Cristina
Walkowicz, L.
author Fontenla, J. M.
author_facet Fontenla, J. M.
Linsky, J. L.
Witbrod, J.
France, K.
Buccino, Andrea Paola
Mauas, Pablo Jacobo David
Vieytes, Mariela Cristina
Walkowicz, L.
author_role author
author2 Linsky, J. L.
Witbrod, J.
France, K.
Buccino, Andrea Paola
Mauas, Pablo Jacobo David
Vieytes, Mariela Cristina
Walkowicz, L.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv planetstar interactions
ultraviolet: stars
stars: late-type
stars: individual: GJ 832
stars: coronae
stars: chromospheres
topic planetstar interactions
ultraviolet: stars
stars: late-type
stars: individual: GJ 832
stars: coronae
stars: chromospheres
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Stellar radiation from X-rays to the visible provides the energy thatcontrols the photochemistry and mass loss from exoplanet atmospheres.The important extreme ultraviolet (EUV) region (10-91.2 nm) isinaccessible and should be computed from a reliable stellar model. It isessential to understand the formation regions and physical processesresponsible for the various stellar emission features to predict how thespectral energy distribution varies with age and activity levels. Wecompute a state-of-the-art semi-empirical atmospheric model and theemergent high-resolution synthetic spectrum of the moderately active M2V star GJ 832 as the first of a series of models for stars withdifferent activity levels. We construct a one-dimensional simple modelfor the physical structure of the star?s chromosphere,chromosphere-corona transition region, and corona using non-LTEradiative transfer techniques and many molecular lines. The synthesizedspectrum for this model fits the continuum and lines across theUV-to-optical spectrum. Particular emphasis is given to the emissionlines at wavelengths that are shorter than 300 nm observed with theHubble Space Telescope, which have important effects on thephotochemistry of the exoplanet atmospheres. The FUV line ratiosindicate that the transition region of GJ 832 is more biased to hottermaterial than that of the quiet Sun. The excellent agreement of ourcomputed EUV luminosity with that obtained by two other techniquesindicates that our model predicts reliable EUV emission from GJ 832. Wefind that the unobserved EUV flux of GJ 832, which heats the outeratmospheres of exoplanets and drives their mass loss, is comparable tothe active Sun.
Fil: Fontenla, J. M.. State University Of Colorado Boulder; Estados Unidos
Fil: Linsky, J. L.. State University Of Colorado Boulder; Estados Unidos
Fil: Witbrod, J.. State University Of Colorado Boulder; Estados Unidos
Fil: France, K.. State University Of Colorado Boulder; Estados Unidos
Fil: Buccino, Andrea Paola. 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: Mauas, Pablo Jacobo David. 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: Vieytes, Mariela Cristina. 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: Walkowicz, L.. The Adler Planetarium; Estados Unidos
description Stellar radiation from X-rays to the visible provides the energy thatcontrols the photochemistry and mass loss from exoplanet atmospheres.The important extreme ultraviolet (EUV) region (10-91.2 nm) isinaccessible and should be computed from a reliable stellar model. It isessential to understand the formation regions and physical processesresponsible for the various stellar emission features to predict how thespectral energy distribution varies with age and activity levels. Wecompute a state-of-the-art semi-empirical atmospheric model and theemergent high-resolution synthetic spectrum of the moderately active M2V star GJ 832 as the first of a series of models for stars withdifferent activity levels. We construct a one-dimensional simple modelfor the physical structure of the star?s chromosphere,chromosphere-corona transition region, and corona using non-LTEradiative transfer techniques and many molecular lines. The synthesizedspectrum for this model fits the continuum and lines across theUV-to-optical spectrum. Particular emphasis is given to the emissionlines at wavelengths that are shorter than 300 nm observed with theHubble Space Telescope, which have important effects on thephotochemistry of the exoplanet atmospheres. The FUV line ratiosindicate that the transition region of GJ 832 is more biased to hottermaterial than that of the quiet Sun. The excellent agreement of ourcomputed EUV luminosity with that obtained by two other techniquesindicates that our model predicts reliable EUV emission from GJ 832. Wefind that the unobserved EUV flux of GJ 832, which heats the outeratmospheres of exoplanets and drives their mass loss, is comparable tothe active Sun.
publishDate 2016
dc.date.none.fl_str_mv 2016-10
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/11336/21732
Fontenla, J. M.; Linsky, J. L.; Witbrod, J.; France, K.; Buccino, Andrea Paola; et al.; Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832; IOP Publishing; Astrophysical Journal; 830; 2; 10-2016; 154,1-18
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21732
identifier_str_mv Fontenla, J. M.; Linsky, J. L.; Witbrod, J.; France, K.; Buccino, Andrea Paola; et al.; Semi-empirical Modeling of the Photosphere, Chromosphere, Transition Region, and Corona of the M-dwarf Host Star GJ 832; IOP Publishing; Astrophysical Journal; 830; 2; 10-2016; 154,1-18
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/0004-637X/830/2/154
info:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/830/2/154
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1608.00934
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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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score 13.070432

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