Rotation period distribution of CoRoT and Kepler Sun-like stars

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dc.contributor.authorLeão, Izan de Castro
dc.contributor.authorPasquini, L.
dc.contributor.authorLopes, C. E. Ferreira
dc.contributor.authorNeves, V.
dc.contributor.authorValcarce, A. A. R.
dc.contributor.authorOliveira, L. L. A. de
dc.contributor.authorSilva, D. Freire da
dc.contributor.authorFreitas, D. B. de
dc.contributor.authorMartins, Bruno Leonardo Canto
dc.contributor.authorJanot-Pacheco, E.
dc.contributor.authorBaglin, A.
dc.contributor.authorMedeiros, José Renan de
dc.date.accessioned2020-05-28T11:59:36Z
dc.date.available2020-05-28T11:59:36Z
dc.date.issued2015
dc.description.resumoAims. 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.pt_BR
dc.identifier.citationMEDEIROS, 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.pt_BR
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201526085
dc.identifier.issn0004-6361 (print), 1432-0746 (online)
dc.identifier.urihttps://repositorio.ufrn.br/jspui/handle/123456789/29081
dc.languageenpt_BR
dc.publisherAstronomy & Astrophysicspt_BR
dc.subjectStars - rotationpt_BR
dc.subjectStars - evolutionpt_BR
dc.subjectStars - solar-typept_BR
dc.subjectSun - rotationpt_BR
dc.titleRotation period distribution of CoRoT and Kepler Sun-like starspt_BR
dc.typearticlept_BR

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