J/MNRAS/491/3586 611 γ Doradus stars Kepler data (Li+, 2020)
Gravity-mode period spacings and near-core rotation rates of 611 γ Doradus
stars with Kepler.
Li G., Van Reeth T., Bedding T.R., Murphy S.J., Antoci V., Ouazzani R.-M.,
Barbara N.H.
<Mon. Not. R. Astron. Soc. 491, 3586-3605 (2020)>
=2020MNRAS.491.3586L 2020MNRAS.491.3586L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, peculiar ; Abundances ; Effective temperatures ; Optical
Keywords: stars: oscillations - stars: rotation
Abstract:
We report our survey of γ Dor stars from the 4-yr Kepler
mission. These stars pulsate mainly in g modes and r modes, showing
period-spacing patterns in the amplitude spectra. The period-spacing
patterns are sensitive to the chemical composition gradients and the
near-core rotation, hence they are essential for understanding the
stellar interior. We identified period-spacing patterns in 611 γ
Dor stars. Almost every star pulsates in dipole g modes, while about
30 per cent of stars also show clear patterns for quadrupole g modes
and 16 per cent of stars present r-mode patterns. We measure periods,
period spacings, and the gradient of the period spacings. These three
observables guide the mode identifications and can be used to estimate
the near-core rotation rate. We find many stars are hotter and show
longer period-spacing patterns than theory. Using the traditional
approximation of rotation (TAR), we inferred the asymptotic spacings,
the near-core rotation rates, and the radial orders of the g and r
modes. Most stars have a near-core rotation rate around 1d-1 and an
asymptotic spacing around 4000s. We also find that many stars rotate
more slowly than predicted by theory for unclear reasons. 11 stars
show rotational splittings with fast rotation rates. We compared the
observed slope-rotation relation with the theory and find a large
spread. We detected rotational modulations in 58 stars and used them
to derive the core-to-surface rotation ratios. The interiors rotate
faster than the cores in most stars, but by no more than 5 per cent.
Description:
We report 957 period-spacing patterns detected from 611 γ Dor
stars, including 22 slow rotators with rotational splittings, 11 rapid
rotators with rotational splittings, 110 stars with r modes, and 58
stars that present surface modulation signals.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 487 957 Sample
table5.dat 59 58 The near-core and surface rotation rates, and
their ratios of 58 stars which show surface
modulation signals
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/A+A/472/241 : UV Flux distributions of gamma Dor stars (Gerbaldi+, 2007)
J/A+A/499/967 : Long-term monitoring of γ Dor stars (Cuypers+, 2009)
J/A+A/556/A52 : γ Dor stars from Kepler (Tkachenko+, 2013)
J/A+A/574/A17 : Period spacings in gamma Dor stars (Van Reeth+, 2015)
J/MNRAS/458/2307 : gamma Dor stars spectroscopic survey
(Kahraman Alicavus+, 2017)
J/A+A/626/A121 : Buoyancy radius of γ Dor stars (Ouazzani+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC KIC number
10- 17 F8.3 --- KICmag KIC magnitude
19- 24 F6.1 --- l Angular degree l, for rossbe modes,
l = k + |m|
26- 31 F6.1 --- m Azimuthal order m
33- 51 F19.17 d Pfirst Period of the first peak
53- 71 F19.17 d Plast Period of the last peak
73- 91 F19.17 d Pmean Mean period
93-113 F21.19 s DeltaPmax Largest period spacing
115-137 F23.20 s DeltaPmin Smallest period spacing
139-160 F22.20 s DeltaPmean Mean period spacing
162-184 E23.20 --- Slope Slope (days/days)
186-207 F22.20 --- e_Slope Slope error (days/days)
209-213 I5 K Teff Effective temperature from DR 25
215-217 I3 K e_Teff Effective temperature error
219-238 F20.16 Lsun L ?=0 Luminosity in solar luminosity
240-260 F21.17 Lsun e_L ?=0 Luminosity error
262-268 F7.2 [-] [Fe/H] ?=9999 Abundance, [Fe/H]
270-276 F7.2 [-] e_[Fe/H] ?=9999 Abundance, Fe/H error
278-281 F4.2 [cm/s2] logg ?=- Surface gravity
283-286 F4.2 [cm/s2] e_logg ?=- Surface gravity error
288-306 F19.13 s Pi0 Asymptotic spacing
308-328 F21.16 s E_Pi0 Asymptotic spacing upper error
330-350 F21.16 s e_Pi0 Asymptotic spacing lower error
352-372 E21.19 d-1 frot Near-core rotation
374-395 F22.20 d-1 E_frot Rotation upper error
397-418 E22.20 d-1 e_frot Rotation lower error
420-423 I4 --- Nmin Minimum radial order
425-428 I4 --- Nmax Maximum radial order
430-436 F7.2 K TeffL ?=0 Effective temperature from LAMOST
438-455 F18.16 [cm/s2] loggL ?=0 Surface gravity from LAMOST
457-479 F23.18 [-] [Fe/H]L ?=9999 Abundance, [Fe/H] from LAMOST
481-487 F7.2 km/s RVL ?=9999 Radial velocity from LAMOST
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [KIC]
5- 12 I8 --- KIC KIC identification number
14- 17 A4 --- Type Type (1)
19- 24 F6.4 d-1 fcore Near-core rotation rate
26- 31 F6.4 d-1 e_fcore rms uncertainty on fcore
33- 38 F6.4 d-1 fsurf Surface rotation rate
40- 45 F6.4 d-1 e_fsurf rms uncertainty on fsurf
47- 52 F6.4 --- fcore/fsurf Near-core to surface rotation rates ratio
54- 59 F6.4 --- e_fcore/fsurf rms uncertainty on fcore/fsurf
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Note (1): Type as follows:
EB = the star is an eclipsing binary
SURF = the signal is caused by surface modulations
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Acknowledgements:
Gang Li, gang.li(at)irap.omp.eu
(End) Patricia Vannier [CDS] 18-May-2021