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
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/67977
Ver los metadatos del registro completo
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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 Técnicas2025-10-22T11:15:18Zoai: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:34982025-10-22 11:15:18.47CONICET 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 |
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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 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa76dd |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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application/pdf application/pdf application/pdf |
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IOP Publishing |
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IOP Publishing |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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