A seismic and gravitationally bound double star observed by Kepler - Implication for the presence of a convective core

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Volume 582 (October 2015)

A&A, 582 (2015) A25

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Table 4

Stellar parameters of the two stars for all the models.

Parameters	Verma	Lebreton	Ball	Creevey	Scaling relations^a

M_A	1.34 ± 0.04	1.25 ± 0.04	1.39 ± 0.02	1.27 ± 0.02	1.27 ± 0.04
M_B	1.11 ± 0.07	1.09 ± 0.02	1.14 ± 0.05	1.08 ± 0.02	1.20 ± 0.06
M_T	2.45 ± 0.08	2.34 ± 0.05	2.53 ± 0.05	2.35 ± 0.03	2.47 ± 0.07
R_A	1.85 ± 0.02	1.82 ± 0.03	1.87 ± 0.01	1.82 ± 0.02	1.82 ± 0.02
R_B	1.24 ± 0.03	1.22 ± 0.02	1.25 ± 0.02	1.23 ± 0.02	1.29 ± 0.02
Age_A (Gyr)	3.50 ± 0.60	3.50 ± 0.20	2.60 ± 0.16	−	3.40 ± 0.30
Age_B (Gyr)	4.10 ± 0.60	4.21 ± 0.29	4.04 ± 0.56	−	4.00 ± 0.60
Age_T (Gyr)	3.80 ± 0.40	3.86 ± 0.35	2.70 ± 0.15	3.35 ± 0.08	3.50 ± 0.30
L_A	4.07 ± 0.20	4.11 ± 0.47	5.50 ± 0.32	4.07 ± 0.13	4.19 ± 0.42
L_B	1.88 ± 0.30	1.98± 0.22	1.99 ± 0.24	1.78 ± 0.10	1.86 ± 0.19
T_eff,A (K)	6020 ± 100	6107	6463 ± 92	6083 ± 13	−
T_eff,B (K)	6070 ± 150	6181	6141 ± 175	6021 ± 50	−
log g_A	4.03	4.02	4.03	4.02 ± 0.007	4.02
log g_B	4.30	4.30	4.32	4.29 ± 0.007	4.30
(Z/X)_0,A	0.026	0.024 ± 0.001	0.022 ± 0.001	0.020	−
(Z/X)_0,B	0.024	0.024 ± 0.003	0.026 ± 0.012	0.020	−
Y_0,A	0.259	0.294 ± 0.014	0.272 ± 0.001	0.271	−
Y_0,B	0.264	0.279 ± 0.007	0.261 ± 0.025	0.271	−
[Fe/H]_A	−0.093	−0.10	−0.16 ± 0.06	−0.13 ± 0.01	−
[Fe/H]_B	−0.082	−0.10	−0.09 ± 0.21	−0.13 ± 0.02	−
α _CONV,A	1.60 (MLT)	0.63 ± 0.02 (CGM)	2.22 ± 0.15 (MLT)	1.91 ± 0.02 (MLT)	−
α _CONV,B	1.72 (MLT)	0.70 ± 0.05 (CGM)	1.84 ± 0.22 (MLT)	1.70 ± 0.17 (MLT)	−
α _OV,A	0.013	0.15	0.014 ± 0.0022	0.10 ± 0.01	−
α _OV,B	0	0	0.005	0	−
R_cc,A (R_⊙)	0.093	0.102	0.108	0.102	−
M_cc,A (M_⊙)	0.079	0.103	0.111	0.101	−
^b	2.88	3.37	1.82	2.30	−
^b	1.43	1.32	1.37	1.39	−
	1.82	2.66	1.79	1.89	−
	1.61	1.88	1.61	2.91	−

Notes.

^(a)

The age is derived from the small frequency separation and the luminosity is from photometry.

^(b)

For getting the number of d.o.f., we computed an SVD decomposition of the covariance matrix C and counted the number of eigenvalues greater than 10^-2 of the largest eigenvalue.

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