Access to Astronomical Catalogues

← Click to display the menu
J/A+A/605/A111      Surface rotation of Kepler red giant stars (Ceillier+, 2017)

Surface rotation of Kepler red giant stars. Ceillier T., Tayar J., Mathur S., Salabert D., Garcia R.A., Stello D., Pinsonneault M.H., van Saders J., Beck P.G., Bloemen S. <Astron. Astrophys. 605, A111 (2017)> =2017A&A...605A.111C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, giant ; Effective temperatures ; Stars, masses Keywords: stars: rotation - stars: activity - stars: evolution Abstract: Kepler allows the measurement of starspot variability in a large sample of field red giants for the first time. With a new method that combines autocorrelation and wavelet decomposition, we measure 361 rotation periods from the full set of 17,377 oscillating red giants in our sample. This represents 2.08% of the stars, consistent with the fraction of spectroscopically detected rapidly rotating giants in the field. The remaining stars do not show enough variability to allow us to measure a reliable surface rotation period. Because the stars with detected rotation periods have measured oscillations, we can infer their global properties, e.g. mass and radius, and quantitatively evaluate the predictions of standard stellar evolution models as a function of mass. Consistent with results for cluster giants, when we consider only the 4881 intermediate-mass stars, M>2.0Mfrom our full red giant sample, we do not find the enhanced rates of rapid rotation one would expect from angular momentum conservation. We therefore suggest that either enhanced angular momentum loss or radial differential rotation must be occurring in these stars. Finally, when we examine the 575 low-mass (M<1.1M) red clump stars in our sample, which we would have expected to exhibit slow (non-detectable) rotation, 15% of them actually have detectable rotation. This suggests a high rate of interactions and stellar mergers on the red giant branch. Description: As only a few red giants are supposed to exhibit light curve modulations due to star spots, we use for this work the largest sample of identified red giants observed by the Kepler satellite so far. It is composed of 17,377 pulsating stars including those already known from previous works (e.g. Huber et al. 2010ApJ...723.1607H; Hekker et al. 2011MNRAS.414.2594H; Mosser et al. 2012A&A...537A..30M; Stello et al. 2013, Cat. J/ApJ/765/L41; Mathur et al. 2016, Cat. J/ApJ/827/50). Table 1 is giving the stars with validated rotation periods. Table 2 is giving the stars showing rotational modulation in their light curve, but probably due to pollution from a nearby star. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 101 361 Stars with validated rotation periods table2.dat 92 170 Stars showing rotational modulation in their light curve, but probably due to pollution from a nearby star
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/ApJ/765/L41 : Asteroseismic classification of KIC objects (Stello+, 2013) J/ApJ/827/50 : Kepler faint red giants (Mathur+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 I8 --- KIC Kepler ID 10- 15 F6.2 uHz numax Frequency of maximum power 17- 21 F5.2 uHz e_numax ?=-1 Error on numax 23- 27 F5.2 uHz dnu Large frequency separation 29- 33 F5.2 uHz e_dnu Error on dnu 35- 38 I4 K Teff Effective Temperature 40- 42 I3 K e_Teff ?=-1 Error on Teff 44- 48 F5.2 [cm/s2] logg Logarithm of the surface gravity 50- 54 F5.2 [cm/s2] e_logg ?=-1 Error on logg 56- 60 F5.2 Msun M Mass of the star 62- 66 F5.2 Msun e_M ?=-1 Error on M 68- 73 F6.2 d Prot Surface Rotation Period 75- 79 F5.2 d e_Prot Error on Prot 81- 84 F4.2 --- Crowding Crowding of the aperture (G1) 86- 90 F5.2 d Tcrit Critical Period 92- 96 F5.2 km/s Vsini Projected velocity 98-101 F4.2 km/s e_Vsini Error on Vsini
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 I8 --- KIC Kepler ID 10- 15 F6.2 muHz numax Frequency of maximum power 17- 21 F5.2 muHz e_numax Error on numax 23- 27 F5.2 muHz dnu Large frequency separation 29- 32 F4.2 muHz e_dnu Error on dnu 34- 38 I5 K Teff Effective Temperature 40- 42 I3 K e_Teff ?=-1 Error on Teff 44- 48 F5.2 [cm/s2] logg Logarithm of the surface gravity 50- 54 F5.2 [cm/s2] e_logg ?=-1 Error on logg 56- 60 F5.2 MSun M Mass of the star 62- 66 F5.2 MSun e_M ?=-1 Error on M 68- 73 F6.2 d Prot Surface Rotation Period 75- 79 F5.2 d e_Prot Error on Prot 81- 84 F4.2 --- Crowding Crowding of the aperture (G1) 86- 90 F5.2 d Tcrit Critical Period 92 I1 --- Flag [1/2] Value of the flag (2)
Note (2): Flag as follows: 1 = star has been discarded because of a low crowding value 2 = star has been discarded because the ratio Prot/Tcrit is too small
Global notes: Note (G1): The crowding value represents the amount of the integrated flux belonging to the targeted star. Hence, it is equal to 1 when only the targeted star is in the aperture.
Acknowledgements: R.A. Garcia, rgarcia(at)cea.fr
(End) R.A. Garcia [Lab. AIM - CEA-DSM - CNRS], P. Vannier [CDS] 25-Jul-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact