The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars
The He » I infrared (IR) line at a vacuum wavelength of 10 833 Å is a diagnostic for the investigation of atmospheres of stars and planets orbiting them. For the first time, we study the behavior of the He » I IR line in a set of chromospheric models for M-dwarf stars, whose much denser chromosphere...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de documento: | artigo |
| Estado: | Versão publicada |
| Data de publicação: | 2020 |
| País: | España |
| Recursos: | Instituto Nacional de Técnica Aeroespacial (INTA) |
| Repositório: | DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
| OAI Identifier: | oai:digital.inta.es:20.500.12666/140 |
| Acesso em linha: | https://www.aanda.org/articles/aa/abs/2020/06/aa37596-20/aa37596-20.html http://hdl.handle.net/20.500.12666/140 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Stars: activity Stars: chromospheres Stars: late-Type |
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The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| title |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| spellingShingle |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars Hintz, D. Stars: activity Stars: chromospheres Stars: late-Type |
| title_short |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| title_full |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| title_fullStr |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| title_full_unstemmed |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| title_sort |
The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars |
| dc.creator.none.fl_str_mv |
Hintz, D. Fuhrmeister, B. Czesla, S. Schmitt, H. M. M. Schweitzer, A. Nagel, E. Johnson, E. N. Caballero, J. A. Zechmeister, M. Jeffers, S. V. Reiners, A. Ribas, I. Amado, P. J. Quirrenbach, A. Anglada Escudé, G. Bauer, F. F. Béjar, V. J. S. Cortés Contreras, M. Dreizler, S. Galadí Enríquez, D. Guenther, E. W. Hauschildt, P. H. Kaminski, A. Kürster, M. Lafarga, M. López del Fresno, M. Montes, D. Morales, J. C. |
| author |
Hintz, D. |
| author_facet |
Hintz, D. Fuhrmeister, B. Czesla, S. Schmitt, H. M. M. Schweitzer, A. Nagel, E. Johnson, E. N. Caballero, J. A. Zechmeister, M. Jeffers, S. V. Reiners, A. Ribas, I. Amado, P. J. Quirrenbach, A. Anglada Escudé, G. Bauer, F. F. Béjar, V. J. S. Cortés Contreras, M. Dreizler, S. Galadí Enríquez, D. Guenther, E. W. Hauschildt, P. H. Kaminski, A. Kürster, M. Lafarga, M. López del Fresno, M. Montes, D. Morales, J. C. |
| author_role |
author |
| author2 |
Fuhrmeister, B. Czesla, S. Schmitt, H. M. M. Schweitzer, A. Nagel, E. Johnson, E. N. Caballero, J. A. Zechmeister, M. Jeffers, S. V. Reiners, A. Ribas, I. Amado, P. J. Quirrenbach, A. Anglada Escudé, G. Bauer, F. F. Béjar, V. J. S. Cortés Contreras, M. Dreizler, S. Galadí Enríquez, D. Guenther, E. W. Hauschildt, P. H. Kaminski, A. Kürster, M. Lafarga, M. López del Fresno, M. Montes, D. Morales, J. C. |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.contributor.none.fl_str_mv |
Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737 0000-0002-5274-2589 0000-0001-6470-2907 0000-0002-6532-4378 0000-0003-1212-5225 Deutsches Zentrum für Luft- und Raumfahrt (DLR) Deutsche Forschungsgemeinschaft (DFG) Agencia Estatal de Investigación (AEI) Ministerio de Economía y Competitividad (MINECO) |
| dc.subject.none.fl_str_mv |
Stars: activity Stars: chromospheres Stars: late-Type |
| topic |
Stars: activity Stars: chromospheres Stars: late-Type |
| description |
The He » I infrared (IR) line at a vacuum wavelength of 10 833 Å is a diagnostic for the investigation of atmospheres of stars and planets orbiting them. For the first time, we study the behavior of the He » I IR line in a set of chromospheric models for M-dwarf stars, whose much denser chromospheres may favor collisions for the level population over photoionization and recombination, which are believed to be dominant in solar-type stars. For this purpose, we use published PHOENIX models for stars of spectral types M2 V and M3 V and also compute new series of models with different levels of activity following an ansatz developed for the case of the Sun. We perform a detailed analysis of the behavior of the He I IR line within these models. We evaluate the line in relation to other chromospheric lines and also the influence of the extreme ultraviolet (EUV) radiation field. The analysis of the He » I IR line strengths as a function of the respective EUV radiation field strengths suggests that the mechanism of photoionization and recombination is necessary to form the line for inactive models, while collisions start to play a role in our most active models. Moreover, the published model set, which is optimized in the ranges of the Na » I D2, Hα, and the bluest Ca » II IR triplet line, gives an adequate prediction of the He » I IR line for most stars of the stellar sample. Because especially the most inactive stars with weak He » I IR lines are fit worst by our models, it seems that our assumption of a 100% filling factor of a single inactive component no longer holds for these stars. © ESO 2020. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020 2021 2021 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 |
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article |
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publishedVersion |
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https://www.aanda.org/articles/aa/abs/2020/06/aa37596-20/aa37596-20.html http://hdl.handle.net/20.500.12666/140 |
| url |
https://www.aanda.org/articles/aa/abs/2020/06/aa37596-20/aa37596-20.html http://hdl.handle.net/20.500.12666/140 |
| dc.language.none.fl_str_mv |
Inglés |
| language_invalid_str_mv |
Inglés |
| dc.relation.none.fl_str_mv |
ENTENDIENDO LA ESTRUCTURA INTERNA, LA EVOLUCION Y LA VARIABILIDAD DE ESTRELLAS DE BAJA MASA CON PLANETAS info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-1-P EXPLOTACION CIENTIFICA DE CARMENES Y PREPARACION DE LOS PROXIMOS BUSCADORES DE EXOPLANETAS ENANAS MARRONES Y PLANETAS AISLADOS Y COMO COMPAÑEROS DE ESTRELLAS PONIENDO LA TIERRA Y EL SISTEMA SOLAR EN CONTEXTO: CIENCIA Y TECNOLOGIA DE CARMENES, CHEOPS, PLATO Y ARIEL ORIGEN Y EVOLUCION DE LAS ENANAS MARRONES Y PLANETAS GIGANTES info:eu-repo/grantAgreement/MINECO//AYA2015-69350-C3-2-P info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2016-80435-C2-1-R info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-2-P info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-3-P |
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Attribution-NonCommercial-NoDerivatives 4.0 International © ESO 2020 https://creativecommons.org/licenses/by-nc-nd/4.0/ info:eu-repo/semantics/openAccess |
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Attribution-NonCommercial-NoDerivatives 4.0 International © ESO 2020 https://creativecommons.org/licenses/by-nc-nd/4.0/ |
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openAccess |
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application/pdf |
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EDP Sciences |
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EDP Sciences |
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reponame:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial instname:Instituto Nacional de Técnica Aeroespacial (INTA) |
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Instituto Nacional de Técnica Aeroespacial (INTA) |
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DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
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DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
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The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V starsHintz, D.Fuhrmeister, B.Czesla, S.Schmitt, H. M. M.Schweitzer, A.Nagel, E.Johnson, E. N.Caballero, J. A.Zechmeister, M.Jeffers, S. V.Reiners, A.Ribas, I.Amado, P. J.Quirrenbach, A.Anglada Escudé, G.Bauer, F. F.Béjar, V. J. S.Cortés Contreras, M.Dreizler, S.Galadí Enríquez, D.Guenther, E. W.Hauschildt, P. H.Kaminski, A.Kürster, M.Lafarga, M.López del Fresno, M.Montes, D.Morales, J. C.Stars: activityStars: chromospheresStars: late-TypeThe He » I infrared (IR) line at a vacuum wavelength of 10 833 Å is a diagnostic for the investigation of atmospheres of stars and planets orbiting them. For the first time, we study the behavior of the He » I IR line in a set of chromospheric models for M-dwarf stars, whose much denser chromospheres may favor collisions for the level population over photoionization and recombination, which are believed to be dominant in solar-type stars. For this purpose, we use published PHOENIX models for stars of spectral types M2 V and M3 V and also compute new series of models with different levels of activity following an ansatz developed for the case of the Sun. We perform a detailed analysis of the behavior of the He I IR line within these models. We evaluate the line in relation to other chromospheric lines and also the influence of the extreme ultraviolet (EUV) radiation field. The analysis of the He » I IR line strengths as a function of the respective EUV radiation field strengths suggests that the mechanism of photoionization and recombination is necessary to form the line for inactive models, while collisions start to play a role in our most active models. Moreover, the published model set, which is optimized in the ranges of the Na » I D2, Hα, and the bluest Ca » II IR triplet line, gives an adequate prediction of the He » I IR line for most stars of the stellar sample. Because especially the most inactive stars with weak He » I IR lines are fit worst by our models, it seems that our assumption of a 100% filling factor of a single inactive component no longer holds for these stars. © ESO 2020.CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Science [through projects AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1-R, AYA2015-69350-C3-2-P, and AYA2018-84089], the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. D.H. acknowledges funding by the DLR under DLR 50 OR1701. B.F. acknowledges funding by the DFG under Cz 222/1-1 and Schm 1032/69-1. S.C. acknowledges support through DFG projects SCH 1382/2-1 and SCHM 1032/66-1. We thank the anonymous referee for the comprehensive review; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).Peer reviewEDP SciencesUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-07370000-0002-5274-25890000-0001-6470-29070000-0002-6532-43780000-0003-1212-5225Deutsches Zentrum für Luft- und Raumfahrt (DLR)Deutsche Forschungsgemeinschaft (DFG)Agencia Estatal de Investigación (AEI)Ministerio de Economía y Competitividad (MINECO)202120212020info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501application/pdfhttps://www.aanda.org/articles/aa/abs/2020/06/aa37596-20/aa37596-20.htmlhttp://hdl.handle.net/20.500.12666/140reponame:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacialinstname:Instituto Nacional de Técnica Aeroespacial (INTA)InglésENTENDIENDO LA ESTRUCTURA INTERNA, LA EVOLUCION Y LA VARIABILIDAD DE ESTRELLAS DE BAJA MASA CON PLANETASinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-1-PEXPLOTACION CIENTIFICA DE CARMENES Y PREPARACION DE LOS PROXIMOS BUSCADORES DE EXOPLANETASENANAS MARRONES Y PLANETAS AISLADOS Y COMO COMPAÑEROS DE ESTRELLASPONIENDO LA TIERRA Y EL SISTEMA SOLAR EN CONTEXTO: CIENCIA Y TECNOLOGIA DE CARMENES, CHEOPS, PLATO Y ARIELORIGEN Y EVOLUCION DE LAS ENANAS MARRONES Y PLANETAS GIGANTESinfo:eu-repo/grantAgreement/MINECO//AYA2015-69350-C3-2-Pinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2016-80435-C2-1-Rinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-2-Pinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-3-PAttribution-NonCommercial-NoDerivatives 4.0 International© ESO 2020https://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:digital.inta.es:20.500.12666/1402026-06-23T12:46:37Z |
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15,300719 |