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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/649
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oai:ri.conicet.gov.ar:11336/649 |
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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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score |
13.070432 |