The relative emission from chromospheres and coronae: Dependence on spectral type and age

Autores
Linsky, Jeffrey L.; Wood, Brian E.; Youngblood, Allison; Brown, Alexander; Froning, Cynthia S.; France, Kevin; Buccino, Andrea Paola; Cranmer, Steven R.; Mauas, Pablo Jacobo David; Miguel, Yamila; Sebastian Pineda, J.; Rugheimer, Sarah; Vieytes, Mariela Cristina; Wheatley, Peter J.; Wilson, David J.
Año de publicación
2020
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Extreme-ultraviolet and X-ray emission from stellar coronae drives mass loss from exoplanet atmospheres, and ultraviolet emission from stellar chromospheres drives photochemistry in exoplanet atmospheres. Comparisons of the spectral energy distributions of host stars are, therefore, essential for understanding the evolution and habitability of exoplanets. The large number of stars observed with the MUSCLES, Mega-MUSCLES, and other recent Hubble Space Telescope observing programs has provided for the first time a large sample (79 stars) of reconstructed Lyα fluxes that we compare with X-ray fluxes to identify significant patterns in the relative emission from these two atmospheric regions as a function of stellar age and effective temperature. We find that as stars age on the main sequence, the emissions from their chromospheres and coronae follow a pattern in response to the amount of magnetic heating in these atmospheric layers. A single trend-line slope describes the pattern of X-ray versus Lyα emission for G and K dwarfs, but the different trend lines for M dwarf stars show that the Lyα fluxes of M stars are significantly smaller than those of warmer stars with the same X-ray flux. The X-ray and Lyα luminosities divided by the stellar bolometric luminosities show different patterns depending on stellar age. The L (Lyα)/L(bol) ratios increase smoothly to cooler stars of all ages, but the L(X)/L(bol) ratios show different trends. For older stars, the increase in coronal emission with decreasing Teff is much steeper than that of chromospheric emission. We suggest a fundamental link between atmospheric properties and trend lines relating coronal and chromospheric heating.
Fil: Linsky, Jeffrey L.. State University of Colorado at Boulder; Estados Unidos
Fil: Wood, Brian E.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
Fil: Youngblood, Allison. State University of Colorado at Boulder; Estados Unidos
Fil: Brown, Alexander. State University of Colorado at Boulder; Estados Unidos
Fil: Froning, Cynthia S.. University of Texas at Austin; Estados Unidos
Fil: France, Kevin. State University of Colorado at Boulder; Estados Unidos
Fil: Buccino, Andrea Paola. Consejo Nacional de Investigaciones 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: Cranmer, Steven R.. State University of Colorado at Boulder; 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. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Miguel, Yamila. Leiden Observatory; Países Bajos
Fil: Sebastian Pineda, J.. State University of Colorado at Boulder; Estados Unidos
Fil: Rugheimer, Sarah. University of Oxford; Reino Unido
Fil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones 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: Wheatley, Peter J.. University of Warwick; Reino Unido
Fil: Wilson, David J.. University of Texas at Austin; Estados Unidos
Materia
Ultraviolet sources
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:11336/182327
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The relative emission from chromospheres and coronae: Dependence on spectral type and ageLinsky, Jeffrey L.Wood, Brian E.Youngblood, AllisonBrown, AlexanderFroning, Cynthia S.France, KevinBuccino, Andrea PaolaCranmer, Steven R.Mauas, Pablo Jacobo DavidMiguel, YamilaSebastian Pineda, J.Rugheimer, SarahVieytes, Mariela CristinaWheatley, Peter J.Wilson, David J.Ultraviolet sourceshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Extreme-ultraviolet and X-ray emission from stellar coronae drives mass loss from exoplanet atmospheres, and ultraviolet emission from stellar chromospheres drives photochemistry in exoplanet atmospheres. Comparisons of the spectral energy distributions of host stars are, therefore, essential for understanding the evolution and habitability of exoplanets. The large number of stars observed with the MUSCLES, Mega-MUSCLES, and other recent Hubble Space Telescope observing programs has provided for the first time a large sample (79 stars) of reconstructed Lyα fluxes that we compare with X-ray fluxes to identify significant patterns in the relative emission from these two atmospheric regions as a function of stellar age and effective temperature. We find that as stars age on the main sequence, the emissions from their chromospheres and coronae follow a pattern in response to the amount of magnetic heating in these atmospheric layers. A single trend-line slope describes the pattern of X-ray versus Lyα emission for G and K dwarfs, but the different trend lines for M dwarf stars show that the Lyα fluxes of M stars are significantly smaller than those of warmer stars with the same X-ray flux. The X-ray and Lyα luminosities divided by the stellar bolometric luminosities show different patterns depending on stellar age. The L (Lyα)/L(bol) ratios increase smoothly to cooler stars of all ages, but the L(X)/L(bol) ratios show different trends. For older stars, the increase in coronal emission with decreasing Teff is much steeper than that of chromospheric emission. We suggest a fundamental link between atmospheric properties and trend lines relating coronal and chromospheric heating.Fil: Linsky, Jeffrey L.. State University of Colorado at Boulder; Estados UnidosFil: Wood, Brian E.. Spece Sciences División. Naval Research Laboratory; Estados UnidosFil: Youngblood, Allison. State University of Colorado at Boulder; Estados UnidosFil: Brown, Alexander. State University of Colorado at Boulder; Estados UnidosFil: Froning, Cynthia S.. University of Texas at Austin; Estados UnidosFil: France, Kevin. State University of Colorado at Boulder; Estados UnidosFil: Buccino, Andrea Paola. Consejo Nacional de Investigaciones 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: Cranmer, Steven R.. State University of Colorado at Boulder; 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. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Miguel, Yamila. Leiden Observatory; Países BajosFil: Sebastian Pineda, J.. State University of Colorado at Boulder; Estados UnidosFil: Rugheimer, Sarah. University of Oxford; Reino UnidoFil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones 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: Wheatley, Peter J.. University of Warwick; Reino UnidoFil: Wilson, David J.. University of Texas at Austin; Estados UnidosIOP Publishing2020-10info: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/11336/182327Linsky, Jeffrey L.; Wood, Brian E.; Youngblood, Allison; Brown, Alexander; Froning, Cynthia S.; et al.; The relative emission from chromospheres and coronae: Dependence on spectral type and age; IOP Publishing; Astrophysical Journal; 902; 1; 10-2020; 1-151538-43570004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abb36finfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abb36finfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2009.01958v1info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:56:24Zoai:ri.conicet.gov.ar:11336/182327instacron: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 09:56:24.268CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The relative emission from chromospheres and coronae: Dependence on spectral type and age
title The relative emission from chromospheres and coronae: Dependence on spectral type and age
spellingShingle The relative emission from chromospheres and coronae: Dependence on spectral type and age
Linsky, Jeffrey L.
Ultraviolet sources
title_short The relative emission from chromospheres and coronae: Dependence on spectral type and age
title_full The relative emission from chromospheres and coronae: Dependence on spectral type and age
title_fullStr The relative emission from chromospheres and coronae: Dependence on spectral type and age
title_full_unstemmed The relative emission from chromospheres and coronae: Dependence on spectral type and age
title_sort The relative emission from chromospheres and coronae: Dependence on spectral type and age
dc.creator.none.fl_str_mv Linsky, Jeffrey L.
Wood, Brian E.
Youngblood, Allison
Brown, Alexander
Froning, Cynthia S.
France, Kevin
Buccino, Andrea Paola
Cranmer, Steven R.
Mauas, Pablo Jacobo David
Miguel, Yamila
Sebastian Pineda, J.
Rugheimer, Sarah
Vieytes, Mariela Cristina
Wheatley, Peter J.
Wilson, David J.
author Linsky, Jeffrey L.
author_facet Linsky, Jeffrey L.
Wood, Brian E.
Youngblood, Allison
Brown, Alexander
Froning, Cynthia S.
France, Kevin
Buccino, Andrea Paola
Cranmer, Steven R.
Mauas, Pablo Jacobo David
Miguel, Yamila
Sebastian Pineda, J.
Rugheimer, Sarah
Vieytes, Mariela Cristina
Wheatley, Peter J.
Wilson, David J.
author_role author
author2 Wood, Brian E.
Youngblood, Allison
Brown, Alexander
Froning, Cynthia S.
France, Kevin
Buccino, Andrea Paola
Cranmer, Steven R.
Mauas, Pablo Jacobo David
Miguel, Yamila
Sebastian Pineda, J.
Rugheimer, Sarah
Vieytes, Mariela Cristina
Wheatley, Peter J.
Wilson, David J.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Ultraviolet sources
topic Ultraviolet sources
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Extreme-ultraviolet and X-ray emission from stellar coronae drives mass loss from exoplanet atmospheres, and ultraviolet emission from stellar chromospheres drives photochemistry in exoplanet atmospheres. Comparisons of the spectral energy distributions of host stars are, therefore, essential for understanding the evolution and habitability of exoplanets. The large number of stars observed with the MUSCLES, Mega-MUSCLES, and other recent Hubble Space Telescope observing programs has provided for the first time a large sample (79 stars) of reconstructed Lyα fluxes that we compare with X-ray fluxes to identify significant patterns in the relative emission from these two atmospheric regions as a function of stellar age and effective temperature. We find that as stars age on the main sequence, the emissions from their chromospheres and coronae follow a pattern in response to the amount of magnetic heating in these atmospheric layers. A single trend-line slope describes the pattern of X-ray versus Lyα emission for G and K dwarfs, but the different trend lines for M dwarf stars show that the Lyα fluxes of M stars are significantly smaller than those of warmer stars with the same X-ray flux. The X-ray and Lyα luminosities divided by the stellar bolometric luminosities show different patterns depending on stellar age. The L (Lyα)/L(bol) ratios increase smoothly to cooler stars of all ages, but the L(X)/L(bol) ratios show different trends. For older stars, the increase in coronal emission with decreasing Teff is much steeper than that of chromospheric emission. We suggest a fundamental link between atmospheric properties and trend lines relating coronal and chromospheric heating.
Fil: Linsky, Jeffrey L.. State University of Colorado at Boulder; Estados Unidos
Fil: Wood, Brian E.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
Fil: Youngblood, Allison. State University of Colorado at Boulder; Estados Unidos
Fil: Brown, Alexander. State University of Colorado at Boulder; Estados Unidos
Fil: Froning, Cynthia S.. University of Texas at Austin; Estados Unidos
Fil: France, Kevin. State University of Colorado at Boulder; Estados Unidos
Fil: Buccino, Andrea Paola. Consejo Nacional de Investigaciones 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: Cranmer, Steven R.. State University of Colorado at Boulder; 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. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Miguel, Yamila. Leiden Observatory; Países Bajos
Fil: Sebastian Pineda, J.. State University of Colorado at Boulder; Estados Unidos
Fil: Rugheimer, Sarah. University of Oxford; Reino Unido
Fil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones 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: Wheatley, Peter J.. University of Warwick; Reino Unido
Fil: Wilson, David J.. University of Texas at Austin; Estados Unidos
description Extreme-ultraviolet and X-ray emission from stellar coronae drives mass loss from exoplanet atmospheres, and ultraviolet emission from stellar chromospheres drives photochemistry in exoplanet atmospheres. Comparisons of the spectral energy distributions of host stars are, therefore, essential for understanding the evolution and habitability of exoplanets. The large number of stars observed with the MUSCLES, Mega-MUSCLES, and other recent Hubble Space Telescope observing programs has provided for the first time a large sample (79 stars) of reconstructed Lyα fluxes that we compare with X-ray fluxes to identify significant patterns in the relative emission from these two atmospheric regions as a function of stellar age and effective temperature. We find that as stars age on the main sequence, the emissions from their chromospheres and coronae follow a pattern in response to the amount of magnetic heating in these atmospheric layers. A single trend-line slope describes the pattern of X-ray versus Lyα emission for G and K dwarfs, but the different trend lines for M dwarf stars show that the Lyα fluxes of M stars are significantly smaller than those of warmer stars with the same X-ray flux. The X-ray and Lyα luminosities divided by the stellar bolometric luminosities show different patterns depending on stellar age. The L (Lyα)/L(bol) ratios increase smoothly to cooler stars of all ages, but the L(X)/L(bol) ratios show different trends. For older stars, the increase in coronal emission with decreasing Teff is much steeper than that of chromospheric emission. We suggest a fundamental link between atmospheric properties and trend lines relating coronal and chromospheric heating.
publishDate 2020
dc.date.none.fl_str_mv 2020-10
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/11336/182327
Linsky, Jeffrey L.; Wood, Brian E.; Youngblood, Allison; Brown, Alexander; Froning, Cynthia S.; et al.; The relative emission from chromospheres and coronae: Dependence on spectral type and age; IOP Publishing; Astrophysical Journal; 902; 1; 10-2020; 1-15
1538-4357
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/182327
identifier_str_mv Linsky, Jeffrey L.; Wood, Brian E.; Youngblood, Allison; Brown, Alexander; Froning, Cynthia S.; et al.; The relative emission from chromospheres and coronae: Dependence on spectral type and age; IOP Publishing; Astrophysical Journal; 902; 1; 10-2020; 1-15
1538-4357
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/https://iopscience.iop.org/article/10.3847/1538-4357/abb36f
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abb36f
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2009.01958v1
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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