Rotation period distribution of CoRoT and Kepler Sun-like stars

Detalhes bibliográficos
Autor(a) principal: Leão, Izan de Castro
Data de Publicação: 2015
Outros Autores: Pasquini, L., Lopes, C. E. Ferreira, Neves, V., Valcarce, A. A. R., Oliveira, L. L. A. de, Silva, D. Freire da, Freitas, D. B. de, Martins, Bruno Leonardo Canto, Janot-Pacheco, E., Baglin, A., Medeiros, José Renan de
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UFRN
Texto Completo: https://repositorio.ufrn.br/jspui/handle/123456789/29081
https://doi.org/10.1051/0004-6361/201526085
Resumo: Aims. We study the distribution of the photometric rotation period (Prot), which is a direct measurement of the surface rotation at active latitudes, for three subsamples of Sun-like stars: one from CoRoT data and two from Kepler data. For this purpose, we identify the main populations of these samples and interpret their main biases specifically for a comparison with the solar Prot. Methods. Prot and variability amplitude (A) measurements were obtained from public CoRoT and Kepler catalogs, which were combined with public data of physical parameters. Because these samples are subject to selection effects, we computed synthetic samples with simulated biases to compare with observations, particularly around the location of the Sun in the Hertzsprung-Russel (HR) diagram. Publicly available theoretical grids and empirical relations were used to combine physical parameters with Prot and A. Biases were simulated by performing cutoffs on the physical and rotational parameters in the same way as in each observed sample. A crucial cutoff is related with the detectability of the rotational modulation, which strongly depends on A. Results. The synthetic samples explain the observed Prot distributions of Sun-like stars as having two main populations: one of young objects (group I, with ages younger than ~1 Gyr) and another of main-sequence and evolved stars (group II, with ages older than ~1 Gyr). The proportions of groups I and II in relation to the total number of stars range within 64–84% and 16–36%, respectively. Hence, young objects abound in the distributions, producing the effect of observing a high number of short periods around the location of the Sun in the HR diagram. Differences in the Prot distributions between the CoRoT and Kepler Sun-like samples may be associated with different Galactic populations. Overall, the synthetic distribution around the solar period agrees with observations, which suggests that the solar rotation is normal with respect to Sun-like stars within the accuracy of current data.
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spelling Leão, Izan de CastroPasquini, L.Lopes, C. E. FerreiraNeves, V.Valcarce, A. A. R.Oliveira, L. L. A. deSilva, D. Freire daFreitas, D. B. deMartins, Bruno Leonardo CantoJanot-Pacheco, E.Baglin, A.Medeiros, José Renan de2020-05-28T11:59:36Z2020-05-28T11:59:36Z2015MEDEIROS, José Renan de et al. Rotation period distribution of CoRoT and Kepler Sun-like stars. Astronomy & Astrophysics (Berlin. Print), v. 582, p. A85, 2015. ISSN 1432-0746 versão online. DOI https://doi.org/10.1051/0004-6361/201526085. Disponível em: https://www.aanda.org/articles/aa/abs/2015/10/aa26085-15/aa26085-15.html. Acesso em: 28 maio 2020. Reproduzido com permissão da Astronomy & Astrophysics, © ESO.0004-6361 (print), 1432-0746 (online)https://repositorio.ufrn.br/jspui/handle/123456789/29081https://doi.org/10.1051/0004-6361/201526085Astronomy & AstrophysicsStars - rotationStars - evolutionStars - solar-typeSun - rotationRotation period distribution of CoRoT and Kepler Sun-like starsinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleAims. We study the distribution of the photometric rotation period (Prot), which is a direct measurement of the surface rotation at active latitudes, for three subsamples of Sun-like stars: one from CoRoT data and two from Kepler data. For this purpose, we identify the main populations of these samples and interpret their main biases specifically for a comparison with the solar Prot. Methods. Prot and variability amplitude (A) measurements were obtained from public CoRoT and Kepler catalogs, which were combined with public data of physical parameters. Because these samples are subject to selection effects, we computed synthetic samples with simulated biases to compare with observations, particularly around the location of the Sun in the Hertzsprung-Russel (HR) diagram. Publicly available theoretical grids and empirical relations were used to combine physical parameters with Prot and A. Biases were simulated by performing cutoffs on the physical and rotational parameters in the same way as in each observed sample. A crucial cutoff is related with the detectability of the rotational modulation, which strongly depends on A. Results. The synthetic samples explain the observed Prot distributions of Sun-like stars as having two main populations: one of young objects (group I, with ages younger than ~1 Gyr) and another of main-sequence and evolved stars (group II, with ages older than ~1 Gyr). The proportions of groups I and II in relation to the total number of stars range within 64–84% and 16–36%, respectively. Hence, young objects abound in the distributions, producing the effect of observing a high number of short periods around the location of the Sun in the HR diagram. Differences in the Prot distributions between the CoRoT and Kepler Sun-like samples may be associated with different Galactic populations. Overall, the synthetic distribution around the solar period agrees with observations, which suggests that the solar rotation is normal with respect to Sun-like stars within the accuracy of current data.engreponame:Repositório Institucional da UFRNinstname:Universidade Federal do Rio Grande do Norte (UFRN)instacron:UFRNinfo:eu-repo/semantics/openAccessORIGINALRotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdfRotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdfapplication/pdf871650https://repositorio.ufrn.br/bitstream/123456789/29081/1/RotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf48d50d4087c1b5010f0d56cdf008c5fbMD51LICENSElicense.txtlicense.txttext/plain; charset=utf-81484https://repositorio.ufrn.br/bitstream/123456789/29081/2/license.txte9597aa2854d128fd968be5edc8a28d9MD52TEXTRotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf.txtRotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf.txtExtracted texttext/plain81746https://repositorio.ufrn.br/bitstream/123456789/29081/3/RotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf.txtef160e78e13fa070a2fc059c6bc0ea16MD53THUMBNAILRotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf.jpgRotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf.jpgGenerated Thumbnailimage/jpeg1673https://repositorio.ufrn.br/bitstream/123456789/29081/4/RotationPeriodDistributionOfCoRoTAndKeplerSun-likeStars_Medeiros_2015.pdf.jpg7ad62385c8bf50fb3606a00d57b45ac1MD54123456789/290812020-06-03 14:30:33.48oai:https://repositorio.ufrn.br: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Repositório de PublicaçõesPUBhttp://repositorio.ufrn.br/oai/opendoar:2020-06-03T17:30:33Repositório Institucional da UFRN - Universidade Federal do Rio Grande do Norte (UFRN)false
dc.title.pt_BR.fl_str_mv Rotation period distribution of CoRoT and Kepler Sun-like stars
title Rotation period distribution of CoRoT and Kepler Sun-like stars
spellingShingle Rotation period distribution of CoRoT and Kepler Sun-like stars
Leão, Izan de Castro
Stars - rotation
Stars - evolution
Stars - solar-type
Sun - rotation
title_short Rotation period distribution of CoRoT and Kepler Sun-like stars
title_full Rotation period distribution of CoRoT and Kepler Sun-like stars
title_fullStr Rotation period distribution of CoRoT and Kepler Sun-like stars
title_full_unstemmed Rotation period distribution of CoRoT and Kepler Sun-like stars
title_sort Rotation period distribution of CoRoT and Kepler Sun-like stars
author Leão, Izan de Castro
author_facet Leão, Izan de Castro
Pasquini, L.
Lopes, C. E. Ferreira
Neves, V.
Valcarce, A. A. R.
Oliveira, L. L. A. de
Silva, D. Freire da
Freitas, D. B. de
Martins, Bruno Leonardo Canto
Janot-Pacheco, E.
Baglin, A.
Medeiros, José Renan de
author_role author
author2 Pasquini, L.
Lopes, C. E. Ferreira
Neves, V.
Valcarce, A. A. R.
Oliveira, L. L. A. de
Silva, D. Freire da
Freitas, D. B. de
Martins, Bruno Leonardo Canto
Janot-Pacheco, E.
Baglin, A.
Medeiros, José Renan de
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.contributor.author.fl_str_mv Leão, Izan de Castro
Pasquini, L.
Lopes, C. E. Ferreira
Neves, V.
Valcarce, A. A. R.
Oliveira, L. L. A. de
Silva, D. Freire da
Freitas, D. B. de
Martins, Bruno Leonardo Canto
Janot-Pacheco, E.
Baglin, A.
Medeiros, José Renan de
dc.subject.por.fl_str_mv Stars - rotation
Stars - evolution
Stars - solar-type
Sun - rotation
topic Stars - rotation
Stars - evolution
Stars - solar-type
Sun - rotation
description Aims. We study the distribution of the photometric rotation period (Prot), which is a direct measurement of the surface rotation at active latitudes, for three subsamples of Sun-like stars: one from CoRoT data and two from Kepler data. For this purpose, we identify the main populations of these samples and interpret their main biases specifically for a comparison with the solar Prot. Methods. Prot and variability amplitude (A) measurements were obtained from public CoRoT and Kepler catalogs, which were combined with public data of physical parameters. Because these samples are subject to selection effects, we computed synthetic samples with simulated biases to compare with observations, particularly around the location of the Sun in the Hertzsprung-Russel (HR) diagram. Publicly available theoretical grids and empirical relations were used to combine physical parameters with Prot and A. Biases were simulated by performing cutoffs on the physical and rotational parameters in the same way as in each observed sample. A crucial cutoff is related with the detectability of the rotational modulation, which strongly depends on A. Results. The synthetic samples explain the observed Prot distributions of Sun-like stars as having two main populations: one of young objects (group I, with ages younger than ~1 Gyr) and another of main-sequence and evolved stars (group II, with ages older than ~1 Gyr). The proportions of groups I and II in relation to the total number of stars range within 64–84% and 16–36%, respectively. Hence, young objects abound in the distributions, producing the effect of observing a high number of short periods around the location of the Sun in the HR diagram. Differences in the Prot distributions between the CoRoT and Kepler Sun-like samples may be associated with different Galactic populations. Overall, the synthetic distribution around the solar period agrees with observations, which suggests that the solar rotation is normal with respect to Sun-like stars within the accuracy of current data.
publishDate 2015
dc.date.issued.fl_str_mv 2015
dc.date.accessioned.fl_str_mv 2020-05-28T11:59:36Z
dc.date.available.fl_str_mv 2020-05-28T11:59:36Z
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dc.type.driver.fl_str_mv info:eu-repo/semantics/article
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dc.identifier.citation.fl_str_mv MEDEIROS, José Renan de et al. Rotation period distribution of CoRoT and Kepler Sun-like stars. Astronomy & Astrophysics (Berlin. Print), v. 582, p. A85, 2015. ISSN 1432-0746 versão online. DOI https://doi.org/10.1051/0004-6361/201526085. Disponível em: https://www.aanda.org/articles/aa/abs/2015/10/aa26085-15/aa26085-15.html. Acesso em: 28 maio 2020. Reproduzido com permissão da Astronomy & Astrophysics, © ESO.
dc.identifier.uri.fl_str_mv https://repositorio.ufrn.br/jspui/handle/123456789/29081
dc.identifier.issn.none.fl_str_mv 0004-6361 (print), 1432-0746 (online)
dc.identifier.doi.none.fl_str_mv https://doi.org/10.1051/0004-6361/201526085
identifier_str_mv MEDEIROS, José Renan de et al. Rotation period distribution of CoRoT and Kepler Sun-like stars. Astronomy & Astrophysics (Berlin. Print), v. 582, p. A85, 2015. ISSN 1432-0746 versão online. DOI https://doi.org/10.1051/0004-6361/201526085. Disponível em: https://www.aanda.org/articles/aa/abs/2015/10/aa26085-15/aa26085-15.html. Acesso em: 28 maio 2020. Reproduzido com permissão da Astronomy & Astrophysics, © ESO.
0004-6361 (print), 1432-0746 (online)
url https://repositorio.ufrn.br/jspui/handle/123456789/29081
https://doi.org/10.1051/0004-6361/201526085
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