The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars

Autores
France, Kevin; Froning, Cynthia S.; Linsky, Jeffrey L.; Roberge, Aki; Stocke, John T.; Tian, Feng; Bushinsky, Rachel; Déser, Jean-Michel; Mauas, Pablo Jacobo David; Vieytes, Mariela Cristina; Walkowicz, Lucianne M.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The spectral and temporal behavior of exoplanet host stars is a critical input to models of the chemistry and evolution of planetary atmospheres. Ultraviolet photons influence the atmospheric temperature profiles and production of potential biomarkers on Earth-like planets around these stars. At present, little observational or theoretical basis exists for understanding the ultraviolet spectra of M dwarfs, despite their critical importance to predicting and interpreting the spectra of potentially habitable planets as they are obtained in the coming decades. Using observations from the Hubble Space Telescope, we present a study of the UV radiation fields around nearby M dwarf planet hosts that covers both far-UV (FUV) and near-UV (NUV) wavelengths. The combined FUV+NUV spectra are publicly available in machine-readable format. We find that all six exoplanet host stars in our sample (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, and GJ 1214) exhibit some level of chromospheric and transition region UV emission. No "UV-quiet" M dwarfs are observed. The bright stellar Lyα emission lines are reconstructed, and we find that the Lyα line fluxes comprise ∼37%-75% of the total 1150-3100 Å flux from most M dwarfs; ≳103 times the solar value. We develop an empirical scaling relation between Lyα and Mg II emission, to be used when interstellar H I attenuation precludes the direct observation of Lyα. The intrinsic unreddened flux ratio is F(Lyα)/F(Mg II) = 10 ± 3. The F(FUV)/F(NUV) flux ratio, a driver for abiotic production of the suggested biomarkers O2 and O3, is shown to be ∼0.5-3 for all M dwarfs in our sample, >103 times the solar ratio. For the four stars with moderate signal-to-noise Cosmic Origins Spectrograph time-resolved spectra, we find UV emission line variability with amplitudes of 50%-500% on 102-103 s timescales. This effect should be taken into account in future UV transiting planet studies, including searches for O 3 on Earth-like planets. Finally, we observe relatively bright H 2 fluorescent emission from four of the M dwarf exoplanetary systems (GJ 581, GJ 876, GJ 436, and GJ 832). Additional modeling work is needed to differentiate between a stellar photospheric or possible exoplanetary origin for the hot (T(H2) ≈ 2000-4000 K) molecular gas observed in these objects.
Fil: France, Kevin. State University of Colorado at Boulder; Estados Unidos
Fil: Froning, Cynthia S.. State University of Colorado at Boulder; Estados Unidos
Fil: Linsky, Jeffrey L.. State University of Colorado at Boulder; Estados Unidos
Fil: Roberge, Aki. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Stocke, John T.. State University of Colorado at Boulder; Estados Unidos
Fil: Tian, Feng. Tsinghua University; China
Fil: Bushinsky, Rachel. State University of Colorado at Boulder; Estados Unidos
Fil: Déser, Jean-Michel. California Institute of Technology; Estados Unidos
Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Walkowicz, Lucianne M.. University of Princeton; Estados Unidos
Materia
PLANETARY SYSTEMS
STARS: ACTIVITY
STARS: INDIVIDUAL (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, GJ 1214)
STARS: LOW-MASS
ULTRAVIOLET: STARS
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:11336/649

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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The Ultraviolet Radiation Environment around M dwarf Exoplanet Host StarsFrance, KevinFroning, Cynthia S.Linsky, Jeffrey L.Roberge, AkiStocke, John T.Tian, FengBushinsky, RachelDéser, Jean-MichelMauas, Pablo Jacobo DavidVieytes, Mariela CristinaWalkowicz, Lucianne M.PLANETARY SYSTEMSSTARS: ACTIVITYSTARS: INDIVIDUAL (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, GJ 1214)STARS: LOW-MASSULTRAVIOLET: STARShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The spectral and temporal behavior of exoplanet host stars is a critical input to models of the chemistry and evolution of planetary atmospheres. Ultraviolet photons influence the atmospheric temperature profiles and production of potential biomarkers on Earth-like planets around these stars. At present, little observational or theoretical basis exists for understanding the ultraviolet spectra of M dwarfs, despite their critical importance to predicting and interpreting the spectra of potentially habitable planets as they are obtained in the coming decades. Using observations from the Hubble Space Telescope, we present a study of the UV radiation fields around nearby M dwarf planet hosts that covers both far-UV (FUV) and near-UV (NUV) wavelengths. The combined FUV+NUV spectra are publicly available in machine-readable format. We find that all six exoplanet host stars in our sample (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, and GJ 1214) exhibit some level of chromospheric and transition region UV emission. No "UV-quiet" M dwarfs are observed. The bright stellar Lyα emission lines are reconstructed, and we find that the Lyα line fluxes comprise ∼37%-75% of the total 1150-3100 Å flux from most M dwarfs; ≳103 times the solar value. We develop an empirical scaling relation between Lyα and Mg II emission, to be used when interstellar H I attenuation precludes the direct observation of Lyα. The intrinsic unreddened flux ratio is F(Lyα)/F(Mg II) = 10 ± 3. The F(FUV)/F(NUV) flux ratio, a driver for abiotic production of the suggested biomarkers O2 and O3, is shown to be ∼0.5-3 for all M dwarfs in our sample, >103 times the solar ratio. For the four stars with moderate signal-to-noise Cosmic Origins Spectrograph time-resolved spectra, we find UV emission line variability with amplitudes of 50%-500% on 102-103 s timescales. This effect should be taken into account in future UV transiting planet studies, including searches for O 3 on Earth-like planets. Finally, we observe relatively bright H 2 fluorescent emission from four of the M dwarf exoplanetary systems (GJ 581, GJ 876, GJ 436, and GJ 832). Additional modeling work is needed to differentiate between a stellar photospheric or possible exoplanetary origin for the hot (T(H2) ≈ 2000-4000 K) molecular gas observed in these objects.Fil: France, Kevin. State University of Colorado at Boulder; Estados UnidosFil: Froning, Cynthia S.. State University of Colorado at Boulder; Estados UnidosFil: Linsky, Jeffrey L.. State University of Colorado at Boulder; Estados UnidosFil: Roberge, Aki. Nasa Goddard Space Flight Center; Estados UnidosFil: Stocke, John T.. State University of Colorado at Boulder; Estados UnidosFil: Tian, Feng. Tsinghua University; ChinaFil: Bushinsky, Rachel. State University of Colorado at Boulder; Estados UnidosFil: Déser, Jean-Michel. California Institute of Technology; Estados UnidosFil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); ArgentinaFil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); ArgentinaFil: Walkowicz, Lucianne M.. University of Princeton; Estados UnidosIOP Publishing2013-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/649France, Kevin; Froning, Cynthia S.; Linsky, Jeffrey L.; Roberge, Aki; Stocke, John T.; et al.; The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars; IOP Publishing; Astrophysical Journal; 763; 149; 2-2013; 149-1630004-637Xenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/763/2/149info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/0004-637X/763/2/149/info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:54:11Zoai:ri.conicet.gov.ar:11336/649instacron: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 09:54:11.621CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
title The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
spellingShingle The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
France, Kevin
PLANETARY SYSTEMS
STARS: ACTIVITY
STARS: INDIVIDUAL (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, GJ 1214)
STARS: LOW-MASS
ULTRAVIOLET: STARS
title_short The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
title_full The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
title_fullStr The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
title_full_unstemmed The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
title_sort The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars
dc.creator.none.fl_str_mv France, Kevin
Froning, Cynthia S.
Linsky, Jeffrey L.
Roberge, Aki
Stocke, John T.
Tian, Feng
Bushinsky, Rachel
Déser, Jean-Michel
Mauas, Pablo Jacobo David
Vieytes, Mariela Cristina
Walkowicz, Lucianne M.
author France, Kevin
author_facet France, Kevin
Froning, Cynthia S.
Linsky, Jeffrey L.
Roberge, Aki
Stocke, John T.
Tian, Feng
Bushinsky, Rachel
Déser, Jean-Michel
Mauas, Pablo Jacobo David
Vieytes, Mariela Cristina
Walkowicz, Lucianne M.
author_role author
author2 Froning, Cynthia S.
Linsky, Jeffrey L.
Roberge, Aki
Stocke, John T.
Tian, Feng
Bushinsky, Rachel
Déser, Jean-Michel
Mauas, Pablo Jacobo David
Vieytes, Mariela Cristina
Walkowicz, Lucianne M.
author2_role author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv PLANETARY SYSTEMS
STARS: ACTIVITY
STARS: INDIVIDUAL (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, GJ 1214)
STARS: LOW-MASS
ULTRAVIOLET: STARS
topic PLANETARY SYSTEMS
STARS: ACTIVITY
STARS: INDIVIDUAL (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, GJ 1214)
STARS: LOW-MASS
ULTRAVIOLET: STARS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The spectral and temporal behavior of exoplanet host stars is a critical input to models of the chemistry and evolution of planetary atmospheres. Ultraviolet photons influence the atmospheric temperature profiles and production of potential biomarkers on Earth-like planets around these stars. At present, little observational or theoretical basis exists for understanding the ultraviolet spectra of M dwarfs, despite their critical importance to predicting and interpreting the spectra of potentially habitable planets as they are obtained in the coming decades. Using observations from the Hubble Space Telescope, we present a study of the UV radiation fields around nearby M dwarf planet hosts that covers both far-UV (FUV) and near-UV (NUV) wavelengths. The combined FUV+NUV spectra are publicly available in machine-readable format. We find that all six exoplanet host stars in our sample (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, and GJ 1214) exhibit some level of chromospheric and transition region UV emission. No "UV-quiet" M dwarfs are observed. The bright stellar Lyα emission lines are reconstructed, and we find that the Lyα line fluxes comprise ∼37%-75% of the total 1150-3100 Å flux from most M dwarfs; ≳103 times the solar value. We develop an empirical scaling relation between Lyα and Mg II emission, to be used when interstellar H I attenuation precludes the direct observation of Lyα. The intrinsic unreddened flux ratio is F(Lyα)/F(Mg II) = 10 ± 3. The F(FUV)/F(NUV) flux ratio, a driver for abiotic production of the suggested biomarkers O2 and O3, is shown to be ∼0.5-3 for all M dwarfs in our sample, >103 times the solar ratio. For the four stars with moderate signal-to-noise Cosmic Origins Spectrograph time-resolved spectra, we find UV emission line variability with amplitudes of 50%-500% on 102-103 s timescales. This effect should be taken into account in future UV transiting planet studies, including searches for O 3 on Earth-like planets. Finally, we observe relatively bright H 2 fluorescent emission from four of the M dwarf exoplanetary systems (GJ 581, GJ 876, GJ 436, and GJ 832). Additional modeling work is needed to differentiate between a stellar photospheric or possible exoplanetary origin for the hot (T(H2) ≈ 2000-4000 K) molecular gas observed in these objects.
Fil: France, Kevin. State University of Colorado at Boulder; Estados Unidos
Fil: Froning, Cynthia S.. State University of Colorado at Boulder; Estados Unidos
Fil: Linsky, Jeffrey L.. State University of Colorado at Boulder; Estados Unidos
Fil: Roberge, Aki. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Stocke, John T.. State University of Colorado at Boulder; Estados Unidos
Fil: Tian, Feng. Tsinghua University; China
Fil: Bushinsky, Rachel. State University of Colorado at Boulder; Estados Unidos
Fil: Déser, Jean-Michel. California Institute of Technology; Estados Unidos
Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Walkowicz, Lucianne M.. University of Princeton; Estados Unidos
description The spectral and temporal behavior of exoplanet host stars is a critical input to models of the chemistry and evolution of planetary atmospheres. Ultraviolet photons influence the atmospheric temperature profiles and production of potential biomarkers on Earth-like planets around these stars. At present, little observational or theoretical basis exists for understanding the ultraviolet spectra of M dwarfs, despite their critical importance to predicting and interpreting the spectra of potentially habitable planets as they are obtained in the coming decades. Using observations from the Hubble Space Telescope, we present a study of the UV radiation fields around nearby M dwarf planet hosts that covers both far-UV (FUV) and near-UV (NUV) wavelengths. The combined FUV+NUV spectra are publicly available in machine-readable format. We find that all six exoplanet host stars in our sample (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, and GJ 1214) exhibit some level of chromospheric and transition region UV emission. No "UV-quiet" M dwarfs are observed. The bright stellar Lyα emission lines are reconstructed, and we find that the Lyα line fluxes comprise ∼37%-75% of the total 1150-3100 Å flux from most M dwarfs; ≳103 times the solar value. We develop an empirical scaling relation between Lyα and Mg II emission, to be used when interstellar H I attenuation precludes the direct observation of Lyα. The intrinsic unreddened flux ratio is F(Lyα)/F(Mg II) = 10 ± 3. The F(FUV)/F(NUV) flux ratio, a driver for abiotic production of the suggested biomarkers O2 and O3, is shown to be ∼0.5-3 for all M dwarfs in our sample, >103 times the solar ratio. For the four stars with moderate signal-to-noise Cosmic Origins Spectrograph time-resolved spectra, we find UV emission line variability with amplitudes of 50%-500% on 102-103 s timescales. This effect should be taken into account in future UV transiting planet studies, including searches for O 3 on Earth-like planets. Finally, we observe relatively bright H 2 fluorescent emission from four of the M dwarf exoplanetary systems (GJ 581, GJ 876, GJ 436, and GJ 832). Additional modeling work is needed to differentiate between a stellar photospheric or possible exoplanetary origin for the hot (T(H2) ≈ 2000-4000 K) molecular gas observed in these objects.
publishDate 2013
dc.date.none.fl_str_mv 2013-02
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/11336/649
France, Kevin; Froning, Cynthia S.; Linsky, Jeffrey L.; Roberge, Aki; Stocke, John T.; et al.; The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars; IOP Publishing; Astrophysical Journal; 763; 149; 2-2013; 149-163
0004-637X
url http://hdl.handle.net/11336/649
identifier_str_mv France, Kevin; Froning, Cynthia S.; Linsky, Jeffrey L.; Roberge, Aki; Stocke, John T.; et al.; The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars; IOP Publishing; Astrophysical Journal; 763; 149; 2-2013; 149-163
0004-637X
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/763/2/149
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/0004-637X/763/2/149/
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 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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