The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs

Autores
Youngblood, Allison; France, Kevin; Loyd, R. O. Parke; Brown, Alexander; Mason, James P.; Schneider, P. Christian; Tilley, Matt A.; Berta-Thompson, Zachory K.; Buccino, Andrea Paola; Froning, Cynthia S.; Hawley, Suzanne L.; Linsky, Jeffrey; Mauas, Pablo Jacobo David; Redfield, Seth; Kowalski, Adam; Miguel, Yamila; Newton, Elisabeth R.; Rugheimer, Sarah; Segura, Antígona; Roberge, Aki; Vieytes, Mariela Cristina
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Characterizing the UV spectral energy distribution (SED) of an exoplanet host star is critically important for assessing its planet´s potential habitability, particularly for M dwarfs, as they are prime targets for current and near-term exoplanet characterization efforts and atmospheric models predict that their UV radiation can produce photochemistry on habitable zone planets different from that on Earth. To derive ground-based proxies for UV emission for use when Hubble Space Telescope (HST) observations are unavailable, we have assembled a sample of 15 early to mid-M dwarfs observed by HST and compared their nonsimultaneous UV and optical spectra. We find that the equivalent width of the chromospheric Ca ii K line at 3933 Å, when corrected for spectral type, can be used to estimate the stellar surface flux in ultraviolet emission lines, including H i Lyα. In addition, we address another potential driver of habitability: energetic particle fluxes associated with flares. We present a new technique for estimating soft X-ray and >10 MeV proton flux during far-UV emission line flares (Si iv and He ii) by assuming solar-like energy partitions. We analyze several flares from the M4 dwarf GJ 876 observed with HST and Chandra as part of the MUSCLES Treasury Survey and find that habitable zone planets orbiting GJ 876 are impacted by large Carrington-like flares with peak soft X-ray fluxes ≥10-3 W m-2 and possible proton fluxes ∼102-103 pfu, approximately four orders of magnitude more frequently than modern-day Earth.
Fil: Youngblood, Allison. University of Colorado; Estados Unidos
Fil: France, Kevin. University of Colorado; Estados Unidos
Fil: Loyd, R. O. Parke. University of Colorado; Estados Unidos
Fil: Brown, Alexander. University of Colorado; Estados Unidos
Fil: Mason, James P.. University of Colorado; Estados Unidos
Fil: Schneider, P. Christian. European Space Research And Technology Centre (esa/estec); Alemania
Fil: Tilley, Matt A.. National Aeronautics and Space Administration; Estados Unidos
Fil: Berta-Thompson, Zachory K.. University of Colorado; Estados Unidos
Fil: Buccino, Andrea Paola. Universidad de Buenos Aires; Argentina. 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: Froning, Cynthia S.. University of Texas at Austin; Estados Unidos
Fil: Hawley, Suzanne L.. University Of Washington, Seattle; Estados Unidos
Fil: Linsky, Jeffrey. University of Colorado; Estados Unidos
Fil: Mauas, Pablo Jacobo David. Universidad de Buenos Aires; Argentina. 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: Redfield, Seth. Wesleyan University Middletown; Reino Unido
Fil: Kowalski, Adam. University of Colorado; Estados Unidos
Fil: Miguel, Yamila. Observatoire de la Cote D'azur; Francia
Fil: Newton, Elisabeth R.. Massachusetts Institute of Technology; Estados Unidos
Fil: Rugheimer, Sarah. University of St. Andrews; Reino Unido
Fil: Segura, Antígona. National Aeronautics and Space Administration; Estados Unidos. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Roberge, Aki. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Vieytes, Mariela Cristina. Universidad de Buenos Aires; Argentina. 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
Materia
STARS: CHROMOSPHERES
STARS: LOW-MASS
SUN: FLARES
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:11336/67977

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spelling The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M DwarfsYoungblood, AllisonFrance, KevinLoyd, R. O. ParkeBrown, AlexanderMason, James P.Schneider, P. ChristianTilley, Matt A.Berta-Thompson, Zachory K.Buccino, Andrea PaolaFroning, Cynthia S.Hawley, Suzanne L.Linsky, JeffreyMauas, Pablo Jacobo DavidRedfield, SethKowalski, AdamMiguel, YamilaNewton, Elisabeth R.Rugheimer, SarahSegura, AntígonaRoberge, AkiVieytes, Mariela CristinaSTARS: CHROMOSPHERESSTARS: LOW-MASSSUN: FLAREShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Characterizing the UV spectral energy distribution (SED) of an exoplanet host star is critically important for assessing its planet´s potential habitability, particularly for M dwarfs, as they are prime targets for current and near-term exoplanet characterization efforts and atmospheric models predict that their UV radiation can produce photochemistry on habitable zone planets different from that on Earth. To derive ground-based proxies for UV emission for use when Hubble Space Telescope (HST) observations are unavailable, we have assembled a sample of 15 early to mid-M dwarfs observed by HST and compared their nonsimultaneous UV and optical spectra. We find that the equivalent width of the chromospheric Ca ii K line at 3933 Å, when corrected for spectral type, can be used to estimate the stellar surface flux in ultraviolet emission lines, including H i Lyα. In addition, we address another potential driver of habitability: energetic particle fluxes associated with flares. We present a new technique for estimating soft X-ray and >10 MeV proton flux during far-UV emission line flares (Si iv and He ii) by assuming solar-like energy partitions. We analyze several flares from the M4 dwarf GJ 876 observed with HST and Chandra as part of the MUSCLES Treasury Survey and find that habitable zone planets orbiting GJ 876 are impacted by large Carrington-like flares with peak soft X-ray fluxes ≥10-3 W m-2 and possible proton fluxes ∼102-103 pfu, approximately four orders of magnitude more frequently than modern-day Earth.Fil: Youngblood, Allison. University of Colorado; Estados UnidosFil: France, Kevin. University of Colorado; Estados UnidosFil: Loyd, R. O. Parke. University of Colorado; Estados UnidosFil: Brown, Alexander. University of Colorado; Estados UnidosFil: Mason, James P.. University of Colorado; Estados UnidosFil: Schneider, P. Christian. European Space Research And Technology Centre (esa/estec); AlemaniaFil: Tilley, Matt A.. National Aeronautics and Space Administration; Estados UnidosFil: Berta-Thompson, Zachory K.. University of Colorado; Estados UnidosFil: Buccino, Andrea Paola. Universidad de Buenos Aires; Argentina. 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: Froning, Cynthia S.. University of Texas at Austin; Estados UnidosFil: Hawley, Suzanne L.. University Of Washington, Seattle; Estados UnidosFil: Linsky, Jeffrey. University of Colorado; Estados UnidosFil: Mauas, Pablo Jacobo David. Universidad de Buenos Aires; Argentina. 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: Redfield, Seth. Wesleyan University Middletown; Reino UnidoFil: Kowalski, Adam. University of Colorado; Estados UnidosFil: Miguel, Yamila. Observatoire de la Cote D'azur; FranciaFil: Newton, Elisabeth R.. Massachusetts Institute of Technology; Estados UnidosFil: Rugheimer, Sarah. University of St. Andrews; Reino UnidoFil: Segura, Antígona. National Aeronautics and Space Administration; Estados Unidos. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoFil: Roberge, Aki. Nasa Goddard Space Flight Center; Estados UnidosFil: Vieytes, Mariela Cristina. Universidad de Buenos Aires; Argentina. 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; ArgentinaIOP Publishing2017-07info: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/11336/67977Youngblood, Allison; France, Kevin; Loyd, R. O. Parke; Brown, Alexander; Mason, James P.; et al.; The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs; IOP Publishing; Astrophysical Journal; 843; 1; 7-2017; 1-510004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa76ddinfo: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:11336/67977instacron: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 09:46:28.97CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
title The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
spellingShingle The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
Youngblood, Allison
STARS: CHROMOSPHERES
STARS: LOW-MASS
SUN: FLARES
title_short The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
title_full The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
title_fullStr The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
title_full_unstemmed The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
title_sort The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs
dc.creator.none.fl_str_mv Youngblood, Allison
France, Kevin
Loyd, R. O. Parke
Brown, Alexander
Mason, James P.
Schneider, P. Christian
Tilley, Matt A.
Berta-Thompson, Zachory K.
Buccino, Andrea Paola
Froning, Cynthia S.
Hawley, Suzanne L.
Linsky, Jeffrey
Mauas, Pablo Jacobo David
Redfield, Seth
Kowalski, Adam
Miguel, Yamila
Newton, Elisabeth R.
Rugheimer, Sarah
Segura, Antígona
Roberge, Aki
Vieytes, Mariela Cristina
author Youngblood, Allison
author_facet Youngblood, Allison
France, Kevin
Loyd, R. O. Parke
Brown, Alexander
Mason, James P.
Schneider, P. Christian
Tilley, Matt A.
Berta-Thompson, Zachory K.
Buccino, Andrea Paola
Froning, Cynthia S.
Hawley, Suzanne L.
Linsky, Jeffrey
Mauas, Pablo Jacobo David
Redfield, Seth
Kowalski, Adam
Miguel, Yamila
Newton, Elisabeth R.
Rugheimer, Sarah
Segura, Antígona
Roberge, Aki
Vieytes, Mariela Cristina
author_role author
author2 France, Kevin
Loyd, R. O. Parke
Brown, Alexander
Mason, James P.
Schneider, P. Christian
Tilley, Matt A.
Berta-Thompson, Zachory K.
Buccino, Andrea Paola
Froning, Cynthia S.
Hawley, Suzanne L.
Linsky, Jeffrey
Mauas, Pablo Jacobo David
Redfield, Seth
Kowalski, Adam
Miguel, Yamila
Newton, Elisabeth R.
Rugheimer, Sarah
Segura, Antígona
Roberge, Aki
Vieytes, Mariela Cristina
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv STARS: CHROMOSPHERES
STARS: LOW-MASS
SUN: FLARES
topic STARS: CHROMOSPHERES
STARS: LOW-MASS
SUN: FLARES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Characterizing the UV spectral energy distribution (SED) of an exoplanet host star is critically important for assessing its planet´s potential habitability, particularly for M dwarfs, as they are prime targets for current and near-term exoplanet characterization efforts and atmospheric models predict that their UV radiation can produce photochemistry on habitable zone planets different from that on Earth. To derive ground-based proxies for UV emission for use when Hubble Space Telescope (HST) observations are unavailable, we have assembled a sample of 15 early to mid-M dwarfs observed by HST and compared their nonsimultaneous UV and optical spectra. We find that the equivalent width of the chromospheric Ca ii K line at 3933 Å, when corrected for spectral type, can be used to estimate the stellar surface flux in ultraviolet emission lines, including H i Lyα. In addition, we address another potential driver of habitability: energetic particle fluxes associated with flares. We present a new technique for estimating soft X-ray and >10 MeV proton flux during far-UV emission line flares (Si iv and He ii) by assuming solar-like energy partitions. We analyze several flares from the M4 dwarf GJ 876 observed with HST and Chandra as part of the MUSCLES Treasury Survey and find that habitable zone planets orbiting GJ 876 are impacted by large Carrington-like flares with peak soft X-ray fluxes ≥10-3 W m-2 and possible proton fluxes ∼102-103 pfu, approximately four orders of magnitude more frequently than modern-day Earth.
Fil: Youngblood, Allison. University of Colorado; Estados Unidos
Fil: France, Kevin. University of Colorado; Estados Unidos
Fil: Loyd, R. O. Parke. University of Colorado; Estados Unidos
Fil: Brown, Alexander. University of Colorado; Estados Unidos
Fil: Mason, James P.. University of Colorado; Estados Unidos
Fil: Schneider, P. Christian. European Space Research And Technology Centre (esa/estec); Alemania
Fil: Tilley, Matt A.. National Aeronautics and Space Administration; Estados Unidos
Fil: Berta-Thompson, Zachory K.. University of Colorado; Estados Unidos
Fil: Buccino, Andrea Paola. Universidad de Buenos Aires; Argentina. 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: Froning, Cynthia S.. University of Texas at Austin; Estados Unidos
Fil: Hawley, Suzanne L.. University Of Washington, Seattle; Estados Unidos
Fil: Linsky, Jeffrey. University of Colorado; Estados Unidos
Fil: Mauas, Pablo Jacobo David. Universidad de Buenos Aires; Argentina. 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: Redfield, Seth. Wesleyan University Middletown; Reino Unido
Fil: Kowalski, Adam. University of Colorado; Estados Unidos
Fil: Miguel, Yamila. Observatoire de la Cote D'azur; Francia
Fil: Newton, Elisabeth R.. Massachusetts Institute of Technology; Estados Unidos
Fil: Rugheimer, Sarah. University of St. Andrews; Reino Unido
Fil: Segura, Antígona. National Aeronautics and Space Administration; Estados Unidos. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Roberge, Aki. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Vieytes, Mariela Cristina. Universidad de Buenos Aires; Argentina. 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
description Characterizing the UV spectral energy distribution (SED) of an exoplanet host star is critically important for assessing its planet´s potential habitability, particularly for M dwarfs, as they are prime targets for current and near-term exoplanet characterization efforts and atmospheric models predict that their UV radiation can produce photochemistry on habitable zone planets different from that on Earth. To derive ground-based proxies for UV emission for use when Hubble Space Telescope (HST) observations are unavailable, we have assembled a sample of 15 early to mid-M dwarfs observed by HST and compared their nonsimultaneous UV and optical spectra. We find that the equivalent width of the chromospheric Ca ii K line at 3933 Å, when corrected for spectral type, can be used to estimate the stellar surface flux in ultraviolet emission lines, including H i Lyα. In addition, we address another potential driver of habitability: energetic particle fluxes associated with flares. We present a new technique for estimating soft X-ray and >10 MeV proton flux during far-UV emission line flares (Si iv and He ii) by assuming solar-like energy partitions. We analyze several flares from the M4 dwarf GJ 876 observed with HST and Chandra as part of the MUSCLES Treasury Survey and find that habitable zone planets orbiting GJ 876 are impacted by large Carrington-like flares with peak soft X-ray fluxes ≥10-3 W m-2 and possible proton fluxes ∼102-103 pfu, approximately four orders of magnitude more frequently than modern-day Earth.
publishDate 2017
dc.date.none.fl_str_mv 2017-07
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/11336/67977
Youngblood, Allison; France, Kevin; Loyd, R. O. Parke; Brown, Alexander; Mason, James P.; et al.; The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs; IOP Publishing; Astrophysical Journal; 843; 1; 7-2017; 1-51
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/67977
identifier_str_mv Youngblood, Allison; France, Kevin; Loyd, R. O. Parke; Brown, Alexander; Mason, James P.; et al.; The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca II K, and Energetic Particle Fluxes from M Dwarfs; IOP Publishing; Astrophysical Journal; 843; 1; 7-2017; 1-51
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/doi/10.3847/1538-4357/aa76dd
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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