Rotation in the Pleiades with K2. II. Multiperiod stars

L. M. Rebull; J. R. Stauffer; J. Bouvier; A. M. Cody; L. A. Hillenbrand; D. R. Soderblom; J. Valenti; D. Barrado; H. Bouy; D. Ciardi; M. Pinsonneault; K. Stassun; G. Micela; S. Aigrain; F. Vrba; G. Somers; E. Gillen; A. Collier Cameron

doi:10.3847/0004-6256/152/5/114

Rotation in the Pleiades with K2. II. Multiperiod stars

L. M. Rebull, J. R. Stauffer, J. Bouvier, A. M. Cody, L. A. Hillenbrand, D. R. Soderblom, J. Valenti, D. Barrado, H. Bouy, D. Ciardi, M. Pinsonneault, K. Stassun, G. Micela, S. Aigrain, F. Vrba, G. Somers, E. Gillen, A. Collier Cameron

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

We use K2 to continue the exploration of the distribution of rotation periods
in Pleiades that we began in Paper I. We have discovered complicated
multi-period behavior in Pleiades stars using these K2 data, and we have
grouped them into categories, which are the focal part of this paper. About 24%
of the sample has multiple, real frequencies in the periodogram, sometimes
manifesting as obvious beating in the light curves. Those having complex and/or structured periodogram peaks, unresolved multiple periods, and resolved close multiple periods are likely due to spot/spot group evolution and/or latitudinal differential rotation; these largely compose the slowly rotating sequence in P versus (V−K_s)₀ identified in Paper I. The fast sequence in P versus (V−K_s)₀ is dominated by single-period stars; these are likely to be rotating as solid bodies. Paper III continues the discussion, speculating about the origin and evolution of the period distribution in the Pleiades.

Original language	English
Article number	114
Number of pages	20
Journal	Astronomical Journal
Volume	152
Issue number	5
DOIs	https://doi.org/10.3847/0004-6256/152/5/114
Publication status	Published - 11 Oct 2016

Keywords

Galaxies: clusters: individual (Pleiades)
Stars: rotation

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Rebull_2016_K2_AstroJ_AAM
© 2016, American Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://dx.doi.org/10.3847/0004-6256/152/5/114
Accepted author manuscript, 4.06 MB

Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018
Jardine, M. M. (PI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Horne, K. D. (CoI) & Wood, K. (CoI)
Science & Technology Facilities Council
1/04/15 → 31/03/18
Project: Standard

Cite this

Rebull, L. M., Stauffer, J. R., Bouvier, J., Cody, A. M., Hillenbrand, L. A., Soderblom, D. R., Valenti, J., Barrado, D., Bouy, H., Ciardi, D., Pinsonneault, M., Stassun, K., Micela, G., Aigrain, S., Vrba, F., Somers, G., Gillen, E., & Cameron, A. C. (2016). Rotation in the Pleiades with K2. II. Multiperiod stars. Astronomical Journal, 152(5), Article 114. https://doi.org/10.3847/0004-6256/152/5/114

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title = "Rotation in the Pleiades with K2. II. Multiperiod stars",

abstract = "We use K2 to continue the exploration of the distribution of rotation periodsin Pleiades that we began in Paper I. We have discovered complicatedmulti-period behavior in Pleiades stars using these K2 data, and we havegrouped them into categories, which are the focal part of this paper. About 24%of the sample has multiple, real frequencies in the periodogram, sometimesmanifesting as obvious beating in the light curves. Those having complex and/or structured periodogram peaks, unresolved multiple periods, and resolved close multiple periods are likely due to spot/spot group evolution and/or latitudinal differential rotation; these largely compose the slowly rotating sequence in P versus (V−Ks)0 identified in Paper I. The fast sequence in P versus (V−Ks)0 is dominated by single-period stars; these are likely to be rotating as solid bodies. Paper III continues the discussion, speculating about the origin and evolution of the period distribution in the Pleiades.",

keywords = "Galaxies: clusters: individual (Pleiades), Stars: rotation",

author = "Rebull, {L. M.} and Stauffer, {J. R.} and J. Bouvier and Cody, {A. M.} and Hillenbrand, {L. A.} and Soderblom, {D. R.} and J. Valenti and D. Barrado and H. Bouy and D. Ciardi and M. Pinsonneault and K. Stassun and G. Micela and S. Aigrain and F. Vrba and G. Somers and E. Gillen and Cameron, {A. Collier}",

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Rebull, LM, Stauffer, JR, Bouvier, J, Cody, AM, Hillenbrand, LA, Soderblom, DR, Valenti, J, Barrado, D, Bouy, H, Ciardi, D, Pinsonneault, M, Stassun, K, Micela, G, Aigrain, S, Vrba, F, Somers, G, Gillen, E & Cameron, AC 2016, 'Rotation in the Pleiades with K2. II. Multiperiod stars', Astronomical Journal, vol. 152, no. 5, 114. https://doi.org/10.3847/0004-6256/152/5/114

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T1 - Rotation in the Pleiades with K2. II. Multiperiod stars

AU - Rebull, L. M.

AU - Stauffer, J. R.

AU - Bouvier, J.

AU - Cody, A. M.

AU - Hillenbrand, L. A.

AU - Soderblom, D. R.

AU - Valenti, J.

AU - Barrado, D.

AU - Bouy, H.

AU - Ciardi, D.

AU - Pinsonneault, M.

AU - Stassun, K.

AU - Micela, G.

AU - Aigrain, S.

AU - Vrba, F.

AU - Somers, G.

AU - Gillen, E.

AU - Cameron, A. Collier

PY - 2016/10/11

Y1 - 2016/10/11

N2 - We use K2 to continue the exploration of the distribution of rotation periodsin Pleiades that we began in Paper I. We have discovered complicatedmulti-period behavior in Pleiades stars using these K2 data, and we havegrouped them into categories, which are the focal part of this paper. About 24%of the sample has multiple, real frequencies in the periodogram, sometimesmanifesting as obvious beating in the light curves. Those having complex and/or structured periodogram peaks, unresolved multiple periods, and resolved close multiple periods are likely due to spot/spot group evolution and/or latitudinal differential rotation; these largely compose the slowly rotating sequence in P versus (V−Ks)0 identified in Paper I. The fast sequence in P versus (V−Ks)0 is dominated by single-period stars; these are likely to be rotating as solid bodies. Paper III continues the discussion, speculating about the origin and evolution of the period distribution in the Pleiades.

AB - We use K2 to continue the exploration of the distribution of rotation periodsin Pleiades that we began in Paper I. We have discovered complicatedmulti-period behavior in Pleiades stars using these K2 data, and we havegrouped them into categories, which are the focal part of this paper. About 24%of the sample has multiple, real frequencies in the periodogram, sometimesmanifesting as obvious beating in the light curves. Those having complex and/or structured periodogram peaks, unresolved multiple periods, and resolved close multiple periods are likely due to spot/spot group evolution and/or latitudinal differential rotation; these largely compose the slowly rotating sequence in P versus (V−Ks)0 identified in Paper I. The fast sequence in P versus (V−Ks)0 is dominated by single-period stars; these are likely to be rotating as solid bodies. Paper III continues the discussion, speculating about the origin and evolution of the period distribution in the Pleiades.

KW - Galaxies: clusters: individual (Pleiades)

KW - Stars: rotation

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DO - 10.3847/0004-6256/152/5/114

M3 - Article

SN - 0004-6256

VL - 152

JO - Astronomical Journal

JF - Astronomical Journal

IS - 5

M1 - 114

ER -

Rotation in the Pleiades with K2. II. Multiperiod stars

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Keywords

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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

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