2018MNRAS.477.5052N


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.16CEST10:30:47

2018MNRAS.477.5052N - Mon. Not. R. Astron. Soc., 477, 5052-5063 (2018/July-2)

Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods.

NSAMBA B., CAMPANTE T.L., MONTEIRO M.J.P.F.G., CUNHA M.S., RENDLE B.M., REESE D.R. and VERMA K.

Abstract (from CDS):

Asteroseismic forward modelling techniques are being used to determine fundamental properties (e.g. mass, radius, and age) of solar-type stars. The need to take into account all possible sources of error is of paramount importance towards a robust determination of stellar properties. We present a study of 34 solar-type stars for which high signal-to-noise asteroseismic data are available from multiyear Kepler photometry. We explore the internal systematics on the stellar properties, that is associated with the uncertainty in the input physics used to construct the stellar models. In particular, we explore the systematics arising from (i) the inclusion of the diffusion of helium and heavy elements; (ii) the uncertainty in solar metallicity mixture; and (iii) different surface correction methods used in optimization/fitting procedures. The systematics arising from comparing results of models with and without diffusion are found to be 0.5 per cent, 0.8 per cent, 2.1 per cent, and 16 per cent in mean density, radius, mass, and age, respectively. The internal systematics in age are significantly larger than the statistical uncertainties. We find the internal systematics resulting from the uncertainty in solar metallicity mixture to be 0.7 per cent in mean density, 0.5 per cent in radius, 1.4 per cent in mass, and 6.7 per cent in age. The surface correction method by Sonoi et al. and Ball & Gizon's two-term correction produce the lowest internal systematics among the different correction methods, namely, ∼1 per cent, ∼1 per cent, ∼2 per cent, and ∼8 per cent in mean density, radius, mass, and age, respectively. Stellar masses obtained using the surface correction methods by Kjeldsen et al. and Ball & Gizon's one-term correction are systematically higher than those obtained using frequency ratios.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): asteroseismology - stars: evolution - stars: fundamental parameters - stars: oscillations

Simbad objects: 35

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Number of rows : 35

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 BD+47 2683 * 18 43 42.4230070169 +47 56 16.007259287   9.85 9.26     G0V 50 0
2 HD 173701 PM* 18 44 35.1192273920 +43 49 59.789089625   8.37 7.52     G8V 121 0
3 BD+43 3102 Ro* 18 51 39.5954267000 +43 38 09.732415288   10.10 9.44     G5V 40 0
4 BD+45 2796 PM* 18 56 21.2644967292 +45 30 53.232987726   9.80 9.29     G0.5IV 61 0
5 HD 176465B * 18 58 03.431 +47 11 29.18   9.24 8.60     ~ 4 0
6 HD 176465 ** 18 58 03.46393 +47 11 30.6471   8.7 8.1     G4V 42 0
7 HD 176465A * 18 58 03.487 +47 11 30.75   9.06 8.47     ~ 5 0
8 HD 176693 Ro* 18 59 08.6846510375 +48 25 23.598982331   9.34 8.83     F8V 87 0
9 TYC 3132-1582-1 * 19 00 06.9396801760 +44 01 45.056884156   11.53 11.05     ~ 17 0
10 HD 177153 PM* 19 01 39.6781881955 +41 29 24.325583971   7.76 7.21     G0 82 0
11 BD+38 3428 PM* 19 05 45.2616790117 +38 31 22.560089042   9.77 9.22     F9IV-V 41 0
12 TYC 3129-1587-1 PM* 19 12 02.2418265719 +42 40 18.806733896   11.49 10.84     ~ 21 0
13 TYC 3121-559-1 * 19 12 16.6298817495 +38 49 03.611425299   10.35 9.75     ~ 24 0
14 TYC 3129-3292-1 * 19 15 08.0776159713 +41 17 55.518976207   11.59 11.00     ~ 17 0
15 BD+39 3706 PM* 19 16 34.9029087477 +40 02 50.362111184       9.1   G1.5V 56 0
16 HD 181207 PM* 19 17 46.3566541779 +41 24 36.837551319   9.06 8.47     F9IV-V 65 0
17 BD+44 3101 PM* 19 18 33.2047287627 +44 24 16.275460206   11.06 10.37     G2V 26 0
18 BD+41 3338 * 19 24 11.1934178701 +42 03 09.726580716   9.97 9.19     G8IV-V 51 0
19 HD 182756 * 19 24 30.3488994710 +40 19 23.671169678   9.01 8.31     G1V 49 0
20 HD 184401 PM* 19 32 14.5965136348 +45 18 38.296572485   9.63 8.95     G5 34 0
21 TYC 3560-2509-1 Ro* 19 33 52.7747006983 +47 02 44.510122069   10.76 10.21     G0V 34 0
22 BD+46 2726 * 19 34 43.0023412508 +46 51 09.934561072   10.36 9.64     K0V 81 0
23 TYC 3135-624-1 PM* 19 36 48.8136899967 +38 42 56.787490867   10.35 9.55     G5IV 53 0
24 BD+44 3197 PM* 19 37 54.5253612516 +44 59 04.628808348       9.3   G0IV 55 0
25 TYC 3556-909-1 PM* 19 37 56.6968956803 +45 57 52.271767840   11.31 10.78     F5 30 0
26 TYC 3556-3445-1 Ro* 19 40 21.2108165107 +45 29 20.960913818   10.48 9.91     G3V 50 0
27 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 664 1
28 * 16 Cyg B PM* 19 41 51.9731830550 +50 31 03.086127222 7.07 6.86 6.20 5.76 5.42 G3V 781 1
29 KOI-364 Ro* 19 43 29.3537343599 +42 52 52.080705146   10.81 10.13     G2.5IVa 46 2
30 BD+43 3349 Ro* 19 45 23.9646013786 +44 04 35.862805965   10.01 9.51     F6IV 29 0
31 TYC 3565-1235-1 PM* 19 45 45.9641996340 +49 59 18.850030411   10.68 9.84     K1V 24 0
32 HD 187160 SB* 19 46 41.3660194374 +44 20 54.685297711   7.650 7.083     F9IV-V 75 0
33 HD 187637 PM* 19 49 18.1388420406 +41 34 56.857643338       7.2   F8V 80 0
34 BD+46 2785 PM* 19 49 19.9798812910 +46 49 36.015004709   9.68 9.21     F2V 18 0
35 HD 190166 PM* 20 01 51.4250664631 +44 21 14.146704965   10.13 9.58     F8V 36 0

    Equat.    Gal    SGal    Ecl

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2019.10.16-10:30:47

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