J/AJ/154/250 Kepler EB classifications and rotation periods (Lurie+, 2017)
Tidal synchronization and differential rotation of Kepler eclipsing binaries.
Lurie J.C., Vyhmeister K., Hawley S.L., Adilia J., Chen A.,
Davenport J.R.A., Juric M., Puig-Holzman M., Weisenburger K.L.
<Astron. J., 154, 250 (2017)>
=2017AJ....154..250L 2017AJ....154..250L (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Stars, late-type
Keywords: binaries: close - binaries: eclipsing - stars: late-type -
stars: oscillations - starspots - stars: rotation
Abstract:
Few observational constraints exist for the tidal synchronization rate
of late-type stars, despite its fundamental role in binary evolution.
We visually inspected the light curves of 2278 eclipsing binaries (EBs)
from the Kepler Eclipsing Binary Catalog to identify those with starspot
modulations, as well as other types of out-of-eclipse variability. We
report rotation periods for 816 EBs with starspot modulations, and find
that 79% of EBs with orbital periods of less than 10 days are synchronized.
However, a population of short-period EBs exists, with rotation periods
typically 13% slower than synchronous, which we attribute to the
differential rotation of high-latitude starspots. At 10 days, there is
a transition from predominantly circular, synchronized EBs to predominantly
eccentric, pseudosynchronized EBs. This transition period is in good
agreement with the predicted and observed circularization period for
Milky Way field binaries. At orbital periods greater than about 30 days,
the amount of tidal synchronization decreases. We also report 12 previously
unidentified candidate δ Scuti and γ Doradus pulsators, as
well as a candidate RS CVn system with an evolved primary that exhibits
starspot occultations. For short-period contact binaries, we observe a
period-color relation and compare it to previous studies. As a whole,
these results represent the largest homogeneous study of tidal
synchronization of late-type stars.
Description:
We began with the 2863 targets in the Kepler Eclipsing Binary Catalog
(KEBC, http://keplerebs.villanova.edu, Prsa et al. 2011, J/AJ/141/83;
Slawson et al. 2011, J/AJ/142/160; Kirk et al. 2016, J/AJ/151/68),
downloaded on 2017 March 24. The KEBC includes orbital periods,
ephemerides, and primary and secondary (when detected) eclipse depths,
widths, and phase separations. After exclusions, there were 2278 EBs
remaining that we analyzed.
Our analysis involved two steps. First, we visually inspected the light
curves to classify EBs with starspot modulations, as well as other types
of EBs. Next, we measured rotation periods for the 816 EBs with starspot
modulations using the following procedure. First, we linearly interpolated
over eclipses, and then measured initial rotation periods using the
autocorrelation function (ACF, see McQuillan et al. 2013, J/MNRAS/432/1203).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 89 2278 EB Classifications and Rotation Periods
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/AJ/141/83 : Kepler Mission. I. Eclipsing binaries in DR1 (Prsa+, 2011)
J/AJ/142/160 : Kepler Mission. II. Eclipsing binaries in DR2
(Slawson+, 2011)
J/MNRAS/432/1203 : Rotation periods of M-dwarf stars (McQuillan+, 2013)
J/AJ/147/45 : Kepler. IV. Eclipse times for close binaries (Conroy+, 2014)
J/PASP/126/914 : Kepler eclipsing binary stars. V. (Conroy+, 2014)
J/MNRAS/448/946 : Kepler eclipse timing variation analyses (Borkovits+, 2015)
J/MNRAS/452/3561 : Kepler eclipsing binary stars. K2 Campaign 0
(LaCourse+, 2015)
J/AJ/151/68 : Kepler Mission. VII. Eclipsing binaries in DR3 (Kirk+, 2016)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [1026032/12785282] Kepler Input Catalog identifier
10- 17 F8.3 d Porb [0.126/1087.3] Orbital period
19- 21 A3 --- Class Visual classification (1)
23- 29 F7.3 d PACF [0.409/199.514]? Autocorrelation function (ACF)
rotation period
31- 35 F5.3 --- hACF [0/1.755]? ACF peak height
37- 42 F6.3 d P1min [0.459/68.277]? First minimum periodogram period
44- 49 F6.3 d P1max [0.46/72.218]? First maximum periodogram period
51- 56 F6.3 d P2min [0.661/33.718]? Second minimum periodogram period
58- 63 F6.3 d P2max [0.662/36.993]? Second maximum periodogram period
65- 69 F5.3 --- h1min [0.003/0.825]? First minimum periodogram height
71- 75 F5.3 --- h1max [0.001/0.749]? First maximum periodogram height
77- 81 F5.3 --- h2min [0.001/0.394]? Second minimum periodogram height
83- 87 F5.3 --- h2max [0.001/0.244]? Second maximum periodogram height
89 A1 --- Note [ab] Note code (2)
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Note (1): Visual classification as follows:
ce = Target where starspot modulations appear to have been mistaken for
ellipsoidal variation. Due to the lack of clear eclipse, this target
may not be EB (see Section 3.1, 6.);
ev = Ellipsoidal variations;
np = No periodic out-of-eclipse variability;
ot = Other out-of-eclipse variability;
pu = Likely pulsator;
pux = Possible pulsator;
sp = Starspot modulations.
Note (2): Note as follows:
a = PACF and hACF for the NP (no periodic out-of-eclipse variability)
category are for validation purposes only, and should not be used for
tidal synchronization analysis;
b = PACF is incorrect due to systematic artifacts in the light curve.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 23-Aug-2018