J/MNRAS/446/2959 Asteroseismology for solar analogues 16 Cyg A/B (Davies+, 2015)
Asteroseismic inference on rotation, gyrochronology and planetary system
dynamics of 16 Cygni.
Davies G.R., Chaplin W.J., Farr W.M., Garcia R.A., Lund M.N., Mathis S.,
Metcalfe T.S., Appourchaux T., Basu S., Benomar O., Campante T.L.,
Ceillier T., Elsworth Y., Handberg R., Salabert D., Stello D.
<Mon. Not. R. Astron. Soc., 446, 2959-2966 (2015)>
=2015MNRAS.446.2959D 2015MNRAS.446.2959D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type ; Stars, double and multiple
Keywords: planet-star interactions - stars: oscillations - stars: rotation
Abstract:
The solar analogues 16 Cyg A and B are excellent asteroseismic targets
in the Kepler field of view and together with a red dwarf and a Jovian
planet form an interesting system. For these more evolved Sun-like
stars we cannot detect surface rotation with the current Kepler data
but instead use the technique of asteroseismology to determine
rotational properties of both 16 Cyg A and B. We find the rotation
periods to be 23.81.5-1.8 and 23.211.5-3.2 d, and the angles
of inclination to be 566-5 ° and 3617-7 °, for A and B,
respectively. Together with these results we use the published mass
and age to suggest that, under the assumption of a solar-like rotation
profile, 16 Cyg A could be used when calibrating gyrochronology
relations. In addition, we discuss the known 16 Cyg B star-planet
eccentricity and measured low obliquity which is consistent with Kozai
cycling and tidal theory.
Description:
Both 16 Cyg A and B are brighter (V∼6) than the saturation limit
for which Kepler observations were designed. However, it was possible
to capture the full stellar flux by using custom photometric aperture
masks. Thus, 928 d of short-cadence observations (Gilliland et al.
2010ApJ...713L.160G 2010ApJ...713L.160G) - from Quarter 7 to 16 - were generated using simple
aperture photometry (Jenkins et al. 2010ApJ...713L..87J 2010ApJ...713L..87J) and then
corrected for instrumental perturbations following the methods
described by Garcia et al. (2011MNRAS.414L...6G 2011MNRAS.414L...6G). The final light
curves used for asteroseismic analyses were high-pass filtered using a
triangular smooth of 4 d width and have a duty cycle of 90.5 per cent.
The power density spectra were computed using a Lomb-Scargle algorithm.
Objects:
---------------------------------------------------------
RA (ICRS) DE Designation(s)
---------------------------------------------------------
19 41 49.09 +50 31 31.6 16 Cyg = IRAS 19404+5024
19 41 48.95 +50 31 30.2 16 Cyg A = KIC 12069424
19 41 51.97 +50 31 03.1 16 Cyg B = KIC 12069449
---------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tables1.dat 17 54 Mode frequencies for 16 Cyg A with 68% credible
regions
tables2.dat 17 56 Mode frequencies for 16 Cyg B with 68% credible
regions
--------------------------------------------------------------------------------
See also:
J/ApJ/737/L32 : Abundances of 16 Cyg A and B (Schuler+, 2011)
J/ApJ/790/L23 : Solar analogs and twins rotation by Kepler
(Do Nascimento+, 2014)
Byte-by-byte Description of file: tables1.dat tables2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- n [12/27] Radial order n
4 I1 --- l [0/3] The degree l of the mode
6- 12 F7.2 10-6Hz Freq Frequency
14- 17 F4.2 10-6Hz Region The 68% credible region
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 02-Nov-2017