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Rotation of Late-type Stars in Praesepe with K2

Rebull, L. M. and Stauffer, J. R. and Hillenbrand, L. A. and Cody, A. M. and Bouvier, J. and Soderblom, D. R. and Pinsonneault, M. and Hebb, L. (2017) Rotation of Late-type Stars in Praesepe with K2. Astrophysical Journal, 839 (2). Art. No. 92. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170420-102625352

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Abstract

We have Fourier-analyzed 941 K2 light curves (LCs) of likely members of Praesepe, measuring periods for 86% and increasing the number of rotation periods (P) by nearly a factor of four. The distribution of P versus (V – K_s), a mass proxy, has three different regimes: (V – K_s) < 1.3, where the rotation rate rapidly slows as mass decreases; 1.3 < (V – K_s) < 4.5, where the rotation rate slows more gradually as mass decreases; and (V – K_s) > 4.5, where the rotation rate rapidly increases as mass decreases. In this last regime, there is a bimodal distribution of periods, with few between ~2 and ~10 days. We interpret this to mean that once M stars start to slow down, they do so rapidly. The K2 period–color distribution in Praesepe (~790 Myr) is much different than that in the Pleiades (~125 Myr) for late F, G, K, and early-M stars; the overall distribution moves to longer periods and is better described by two line segments. For mid-M stars, the relationship has a similarly broad scatter and is steeper in Praesepe. The diversity of LCs and of periodogram types is similar in the two clusters; about a quarter of the periodic stars in both clusters have multiple significant periods. Multi-periodic stars dominate among the higher masses, starting at a bluer color in Praesepe ((V – K_s) ~ 1.5) than in the Pleiades ((V – K_s) ~ 2.6). In Praesepe, there are relatively more LCs that have two widely separated periods, ΔP > 6 days. Some of these could be examples of M star binaries where one star has spun down but the other has not.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa6aa4DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa6aa4/metaPublisherArticle
https://arxiv.org/abs/1703.07031arXivDiscussion Paper
ORCID:
AuthorORCID
Rebull, L. M.0000-0001-6381-515X
Stauffer, J. R.0000-0003-3595-7382
Cody, A. M.0000-0002-3656-6706
Bouvier, J.0000-0002-7450-6712
Soderblom, D. R.0000-0002-0322-8161
Pinsonneault, M.0000-0002-7549-7766
Hebb, L.0000-0003-1263-8637
Additional Information:© 2017 The American Astronomical Society. Received 2017 January 30; revised 2017 March 14; accepted 2017 March 20; published 2017 April 20. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This research has made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, and of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of data products from the Two Micron All-Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. The 2MASS data are served by the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Facilities: Kepler - The Kepler Mission, K2 - , 2MASS.
Group:Infrared Processing and Analysis Center (IPAC), Astronomy Department
Funders:
Funding AgencyGrant Number
NASANNX09AF08G
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:stars: rotation – stars: variables: general
Issue or Number:2
Record Number:CaltechAUTHORS:20170420-102625352
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170420-102625352
Official Citation:L. M. Rebull et al 2017 ApJ 839 92
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:76758
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:20 Apr 2017 18:46
Last Modified:09 Mar 2020 13:18

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