J/MNRAS/436/1883 Properties of KOI host stars (Walkowicz+, 2013)
Rotation periods, variability properties and ages for Kepler exoplanet
candidate host stars.
Walkowicz L.M., Basri G.S.
<Mon. Not. R. Astron. Soc., 436, 1883-1895 (2013)>
=2013MNRAS.436.1883W 2013MNRAS.436.1883W
ADC_Keywords: Stars, double and multiple ; Planets ; Stars, ages ;
Effective temperatures
Keywords: stars: activity - planetary systems - stars: rotation
Abstract:
We report rotation periods, variability characteristics,
gyrochronological ages for ∼950 of the Kepler Object of
Interest host stars. We find a wide dispersion in the amplitude of the
photometric variability as a function of rotation, likely indicating
differences in the spot distribution among stars. We use these
rotation periods in combination with published spectroscopic
measurements of vsini and stellar parameters to derive
the stellar inclination in the line of sight, and find a number of
systems with possible spin-orbit misalignment. We additionally find
several systems with close-in planet candidates whose stellar rotation
periods are equal to or twice the planetary orbital period, indicative
of possible tidal interactions between these planets and their parent
stars. If these systems survive validation to become confirmed
planets, they will provide important clues to the evolutionary history
of these systems.
Description:
We chose to work with the light curves from Kepler Quarter 9, as this
was the first quarter reduced using the PDC-MAP detrending pipeline
(previous quarters have since been reprocessed, such that all Kepler
data have now been detrended using PDC-MAP).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 64 954 Periods and variability for
Kepler Objects of Interest
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/ApJS/210/19 : Kepler planetary candidates. IV. 22 months (Burke+, 2014)
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 Kepler ID (Cat. V/133)
10- 13 I4 --- KOI [8/3136] KOI identification number
15- 18 I4 K Teff ?=-99 Effective temperature
20- 25 F6.2 [cm/s2] logg [3/5.1]?=-99 Gravity surface
27- 31 F5.2 [10-3] logVar Variability range (in parts per thousand, ppt)
33- 37 F5.2 d Per [0/44] Period
39- 43 F5.2 d e_Per rms uncertainty on Per (1)
45- 50 F6.2 --- Ro [0/6]?=-99 Rossby number (P/τc (3)
52- 57 F6.2 mag B-V [0/4]?=-99 B-V colour index
59- 64 F6.2 Gyr Age [0/15]?=-99 Age prediction (2)
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Note (1): Period uncertainties provided are taken as the half-width
half-maximum of a gaussian with the same peak height and integrated
area as the periodogram peak nearest the adopted period. These widths
are largely a function of the periodogram sampling (longer periods
tend to have wider peaks) and so are overestimates of the uncertainty
in the period, but are provided here for completeness.
For hotter stars (Teff>6200K) that are not expected to possess a solar-like
magnetic dynamo, periodicities may be due to ellipsoidal variations or
pulsations rather than rotational modulation by stellar magnetic features.
Note (2): Gyrochronological ages are provided for all objects having B-V>0.5
and Teff<6200K, but the reader is advised that these ages are highly
uncertain for very young stars (P<10days) and cool stars.
Note (3): the Rossby number (P/τc) is the ratio between the rotation
period P and the convective turnover time τc.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Oct-2014