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Stellar rotational periods in the planet hosting open cluster Praesepe

Author(s): Kovács, Géza; Hartman, Joel D; Bakos, Gaspar Aron; Quinn, Samuel N; Penev, Kaloyan; et al

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dc.contributor.authorKovács, Géza-
dc.contributor.authorHartman, Joel D-
dc.contributor.authorBakos, Gaspar Aron-
dc.contributor.authorQuinn, Samuel N-
dc.contributor.authorPenev, Kaloyan-
dc.contributor.authorLatham, David W-
dc.contributor.authorBhatti, Waqas-
dc.contributor.authorCsubry, Zoltán-
dc.contributor.authorde Val-Borro, Miguel-
dc.date.accessioned2019-04-10T19:31:24Z-
dc.date.available2019-04-10T19:31:24Z-
dc.date.issued2014-08-11en_US
dc.identifier.citationKovács, Géza, Hartman, Joel D, Bakos, Gáspár Á, Quinn, Samuel N, Penev, Kaloyan, Latham, David W, Bhatti, Waqas, Csubry, Zoltán, de Val-Borro, Miguel. (2014). Stellar rotational periods in the planet hosting open cluster Praesepe. \mnras, 442 (2081 - 2093. doi:10.1093/mnras/stu946en_US
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr1gq5k-
dc.description.abstractBy using the dense coverage of the extrasolar planet survey project HATNet (Hungarian-made Automated Telescope Network), we Fourier analyse 381 high-probability members of the nearby open cluster Praesepe (Beehive/M44/NGC 2632). In addition to the detection of 10 variables (of δ Scuti and other types), we identify 180 rotational variables (including the two known planet hosts). This sample increases the number of known rotational variables in this cluster for spectral classes earlier than M by more than a factor of 3. These stars closely follow a colour/magnitude–period relation from early F to late K stars. We approximate this relation by polynomials for an easier reference to the rotational characteristics in different colours. The total (peak-to-peak) amplitudes of the large majority (94 per cent) of these variables span the range of 0.005–0.04 mag. The periods cover a range from 2.5 to 15 d. These data strongly confirm that Praesepe and the Hyades have the same gyrochronological ages. Regarding the two planet hosts, Pr0211 (the one with the shorter orbital period) has a rotational period that is ∼2 d shorter than the one expected from the main rotational pattern in this cluster. This, together with other examples discussed in the paper, may hint that star–planet interaction via tidal dissipation can be significant in some cases in the rotational evolution of stars hosting hot Jupiters.en_US
dc.format.extent2081 - 2093en_US
dc.language.isoen_USen_US
dc.relation.ispartofMonthly notices of the Royal Astronomical Society.en_US
dc.rightsFinal published version. Article is made available in OAR by the publisher's permission or policy.en_US
dc.titleStellar rotational periods in the planet hosting open cluster Praesepeen_US
dc.typeJournal Articleen_US
dc.identifier.doidoi:10.1093/mnras/stu946-
dc.date.eissued2014-06-18en_US
pu.type.symplectichttp://www.symplectic.co.uk/publications/atom-terms/1.0/journal-articleen_US

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