The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars
Due to their ubiquity and very long main-sequence lifetimes, abundance determinations in M dwarfs provide a powerful and alternative tool to GK dwarfs to study the formation and chemical enrichment history of our Galaxy. In this study, abundances of the neutron-capture elements Rb, Sr, and Zr are de...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2020 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/223731 |
| Acceso en línea: | http://hdl.handle.net/10261/223731 |
| Access Level: | acceso abierto |
| Palabra clave: | Nuclear reactions Stars: late-type Stars: abundances Nucleosynthesis |
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oai:digital.csic.es:10261/223731 |
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The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| title |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| spellingShingle |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars Abia, C. Nuclear reactions Stars: late-type Stars: abundances Nucleosynthesis |
| title_short |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| title_full |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| title_fullStr |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| title_full_unstemmed |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| title_sort |
The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars |
| dc.creator.none.fl_str_mv |
Abia, C. Tabernero, H. M. Korotin, S. A. Montes, David Marfil, E. Caballero, J. A. Straniero, O. Prantzos, Nikos Ribas, Ignasi Reiners, Ansgar Quirrenbach, Andreas Amado, Pedro J. Béjar, Victor J. S. Cortés-Contreras, M. Dreizler, Stefan Henning, Thomas Jeffers, Sandra V. Kaminski, Adrian Kürster, M. Lafarga, M. López-Gallifa, Á. Morales, Juan Carlos Nagel, Evangelos Passegger, V.M. Pedraz, S. Rodríguez-López, Cristina Schweitzer, Andreas Zechmeister, Mathias |
| author |
Abia, C. |
| author_facet |
Abia, C. Tabernero, H. M. Korotin, S. A. Montes, David Marfil, E. Caballero, J. A. Straniero, O. Prantzos, Nikos Ribas, Ignasi Reiners, Ansgar Quirrenbach, Andreas Amado, Pedro J. Béjar, Victor J. S. Cortés-Contreras, M. Dreizler, Stefan Henning, Thomas Jeffers, Sandra V. Kaminski, Adrian Kürster, M. Lafarga, M. López-Gallifa, Á. Morales, Juan Carlos Nagel, Evangelos Passegger, V.M. Pedraz, S. Rodríguez-López, Cristina Schweitzer, Andreas Zechmeister, Mathias |
| author_role |
author |
| author2 |
Tabernero, H. M. Korotin, S. A. Montes, David Marfil, E. Caballero, J. A. Straniero, O. Prantzos, Nikos Ribas, Ignasi Reiners, Ansgar Quirrenbach, Andreas Amado, Pedro J. Béjar, Victor J. S. Cortés-Contreras, M. Dreizler, Stefan Henning, Thomas Jeffers, Sandra V. Kaminski, Adrian Kürster, M. Lafarga, M. López-Gallifa, Á. Morales, Juan Carlos Nagel, Evangelos Passegger, V.M. Pedraz, S. Rodríguez-López, Cristina Schweitzer, Andreas Zechmeister, Mathias |
| 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 |
Ministerio de Ciencia e Innovación (España) European Commission Universidad Complutense de Madrid Fundação para a Ciência e a Tecnologia (Portugal) NASA Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Nuclear reactions Stars: late-type Stars: abundances Nucleosynthesis |
| topic |
Nuclear reactions Stars: late-type Stars: abundances Nucleosynthesis |
| description |
Due to their ubiquity and very long main-sequence lifetimes, abundance determinations in M dwarfs provide a powerful and alternative tool to GK dwarfs to study the formation and chemical enrichment history of our Galaxy. In this study, abundances of the neutron-capture elements Rb, Sr, and Zr are derived, for the first time, in a sample of nearby M dwarfs. We focus on stars in the metallicity range-0.5 ≲ [Fe/H] ≲ +0.3, an interval poorly explored for Rb abundances in previous analyses. To do this we use high-resolution, high-signal-to-noise-ratio, optical and near-infrared spectra of 57 M dwarfs observed with CARMENES. The resulting [Sr/Fe] and [Zr/Fe] ratios for most M dwarfs are almost constant at about the solar value, and are identical to those found in GK dwarfs of the same metallicity. However, for Rb we find systematic underabundances ([Rb/Fe] < 0.0) by a factor two on average. Furthermore, a tendency is found for Rb-but not for other heavy elements (Sr, Zr)-to increase with increasing metallicity such that [Rb/Fe] ≳ 0.0 is attained at metallicities higher than solar. These are surprising results, never seen for any other heavy element, and are difficult to understand within the formulation of the s-and r-processes, both contributing sources to the Galactic Rb abundance. We discuss the reliability of these findings for Rb in terms of non-LTE (local thermodynamic equilibrium) effects, stellar activity, or an anomalous Rb abundance in the Solar System, but no explanation is found. We then interpret the full observed [Rb/Fe] versus [Fe/H] trend within the framework of theoretical predictions from state-of-the-art chemical evolution models for heavy elements, but a simple interpretation is not found either. In particular, the possible secondary behaviour of the [Rb/Fe] ratio at super-solar metallicities would require a much larger production of Rb than currently predicted in AGB stars through the s-process without overproducing Sr and Zr. © 2020 ESO. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020 2020 2020 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/223731 |
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http://hdl.handle.net/10261/223731 |
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Inglés |
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Inglés |
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The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool starsAbia, C.Tabernero, H. M.Korotin, S. A.Montes, DavidMarfil, E.Caballero, J. A.Straniero, O.Prantzos, NikosRibas, IgnasiReiners, AnsgarQuirrenbach, AndreasAmado, Pedro J.Béjar, Victor J. S.Cortés-Contreras, M.Dreizler, StefanHenning, ThomasJeffers, Sandra V.Kaminski, AdrianKürster, M.Lafarga, M.López-Gallifa, Á.Morales, Juan CarlosNagel, EvangelosPassegger, V.M.Pedraz, S.Rodríguez-López, CristinaSchweitzer, AndreasZechmeister, MathiasNuclear reactionsStars: late-typeStars: abundancesNucleosynthesisDue to their ubiquity and very long main-sequence lifetimes, abundance determinations in M dwarfs provide a powerful and alternative tool to GK dwarfs to study the formation and chemical enrichment history of our Galaxy. In this study, abundances of the neutron-capture elements Rb, Sr, and Zr are derived, for the first time, in a sample of nearby M dwarfs. We focus on stars in the metallicity range-0.5 ≲ [Fe/H] ≲ +0.3, an interval poorly explored for Rb abundances in previous analyses. To do this we use high-resolution, high-signal-to-noise-ratio, optical and near-infrared spectra of 57 M dwarfs observed with CARMENES. The resulting [Sr/Fe] and [Zr/Fe] ratios for most M dwarfs are almost constant at about the solar value, and are identical to those found in GK dwarfs of the same metallicity. However, for Rb we find systematic underabundances ([Rb/Fe] < 0.0) by a factor two on average. Furthermore, a tendency is found for Rb-but not for other heavy elements (Sr, Zr)-to increase with increasing metallicity such that [Rb/Fe] ≳ 0.0 is attained at metallicities higher than solar. These are surprising results, never seen for any other heavy element, and are difficult to understand within the formulation of the s-and r-processes, both contributing sources to the Galactic Rb abundance. We discuss the reliability of these findings for Rb in terms of non-LTE (local thermodynamic equilibrium) effects, stellar activity, or an anomalous Rb abundance in the Solar System, but no explanation is found. We then interpret the full observed [Rb/Fe] versus [Fe/H] trend within the framework of theoretical predictions from state-of-the-art chemical evolution models for heavy elements, but a simple interpretation is not found either. In particular, the possible secondary behaviour of the [Rb/Fe] ratio at super-solar metallicities would require a much larger production of Rb than currently predicted in AGB stars through the s-process without overproducing Sr and Zr. © 2020 ESO.CARMENES is an instrument for the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisica de Andalucia (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Cientificas (CSIC), the Ministerio de Economia y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, 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 MINECO, the Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme and 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. We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia e Innovacion, the Universidad Complutense de Madrid, the Fundacao para a Ciencia e a Tecnologia, the Generalitat de Catalunya, ERDF, and NASA through projects PGC2018-095317-B-C21, PID2019-109522GB-C51/2/3/4, PGC2018-098153-B-C33, AYA2016-79425-C3[1,2,3]-P, FPU15/01476, UID[B,P]/04434/2020, PTDC/FIS-AST/28953/2017, POCI-01-0145-FEDER-028953, SEV-2015-0548, SEV-2017-0709, MDM-20170737, NNX17AG24G, and the CERCA programme.Peer reviewedEDP SciencesMinisterio de Ciencia e Innovación (España)European CommissionUniversidad Complutense de MadridFundação para a Ciência e a Tecnologia (Portugal)NASAConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202020202020info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/223731reponame:DIGITAL.CSIC. 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