Rotation period distribution of CoRoT and Kepler Sun-like stars
Autor(a) principal: | |
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Data de Publicação: | 2015 |
Outros Autores: | , , , , , , , , , , |
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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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 |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
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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eng |
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eng |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
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openAccess |
dc.publisher.none.fl_str_mv |
Astronomy & Astrophysics |
publisher.none.fl_str_mv |
Astronomy & Astrophysics |
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reponame:Repositório Institucional da UFRN instname:Universidade Federal do Rio Grande do Norte (UFRN) instacron:UFRN |
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UFRN |
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