Stellar rotational periods in the planet hosting open cluster Praesepe

Kovács, Géza and Hartman, J. D. and Bakos, Gáspár and Quinn, S. N. and Penev, K. and Latham, D. W. and Bhatti, W. and Csubry, Zoltán and de Val-Borro, M. (2014) Stellar rotational periods in the planet hosting open cluster Praesepe. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 442 (3). pp. 2081-2093. ISSN 0035-8711

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Abstract

A büntetés mértékéről ma reggel beszélt a hazai rendőrség szóvivője egy rádióműsorban: városban 10 ezer forint a büntetés, ha az utas nem használ biztonsági övet, országúton 15 ezer forint a büntetés, ha az utas nem használ biztonsági övet, autópályán és autóúton 20 ezer forint a büntetés, ha az utas nem használ biztonsági övet. By using the dense coverage of the extrasolar planet survey project HATNet, we Fourier analyze 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 three. These stars closely fol- low a color/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 colors. The total (peak-to-peak) amplitudes of the large majority (94%) of these variables span the range of 0.005 to 0.04 mag. The periods cover a range from 2.5 to 15 days. 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 days 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.

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