2014A&A...566A..20A


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST21:57:43

2014A&A...566A..20A - Astronomy and Astrophysics, volume 566A, 20-20 (2014/6-1)

Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler.

APPOURCHAUX T., ANTIA H.M., BENOMAR O., CAMPANTE T.L., DAVIES G.R., HANDBERG R., HOWE R., REGULO C., BELKACEM K., HOUDEK G., GARCIA R.A. and CHAPLIN W.J.

Abstract (from CDS):

Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe the stars using asteroseismology. We provide the mode linewidths and mode heights of the oscillations of various stars as a function of frequency and of effective temperature. We used a time series of nearly two years of data for each star. The 23 stars observed belong to the simple or F-like category. The power spectra of the 23 main-sequence stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We study the source of systematic errors in the mode linewidths and mode heights, and we present a way to correct these errors with respect to a common reference fit. Using the correction, we can explain all sources of systematic errors, which could be reduced to less than ±15% for mode linewidths and heights, and less than ±5% for amplitude, when compared to the reference fit. The effect of a different estimated stellar background and a different estimated splitting will provide frequency-dependent systematic errors that might affect the comparison with theoretical mode linewidth and mode height, therefore affecting the understanding of the physical nature of these parameters. All other sources of relative systematic errors are less dependent upon frequency. We also provide the dependence of the so-called linewidth dip in the middle of the observed frequency range as a function of effective temperature. We show that the depth of the dip decreases with increasing effective temperature. The dependence of the dip on effective temperature may imply that the mixing length parameter α or the convective flux may increase with effective temperature.

Abstract Copyright:

Journal keyword(s): stars: interiors - asteroseismology - methods: data analysis

Errata: erratum vol. 595, art. C2 (2016)

Simbad objects: 27

goto Full paper

goto View the reference in ADS

Number of rows : 27

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 BD+46 2555 Ro* 18 47 39.2488304951 +46 41 09.978990968   9.98 9.52     F6IV 41 0
2 BD+45 2796 PM* 18 56 21.2644967292 +45 30 53.232987726   9.80 9.29     G0.5IV 67 0
3 HD 176071 PM* 18 56 22.1269692202 +45 30 25.359126300   8.81 8.33     F8IV 68 0
4 HD 176153 Ro* 18 56 36.6478619140 +47 39 23.163197712   9.20 8.68     F9IV-V 65 0
5 TYC 3120-180-1 * 19 00 42.9751738603 +38 34 24.882641980   10.33 9.84     G0IV 20 0
6 HD 177723 * 19 03 45.1359001568 +45 36 30.188777836   9.54 9.10     F8IV 46 0
7 TYC 3545-1033-1 * 19 04 45.6028236992 +48 21 33.385044320   11.54 11.00     F6IV 20 0
8 HD 178509 Ro* 19 06 55.9483071065 +42 40 19.337596523   9.39 8.86     F8IV 43 0
9 HD 178688 * 19 07 43.5917073663 +41 56 15.729857285   9.48 9.02     F6IV 35 0
10 HD 178971 Ro* 19 09 01.9440013031 +38 53 59.483977067   8.79 8.36     F5IV-V 52 0
11 HD 179260 * 19 10 11.6374335186 +38 04 55.826877281   8.94 8.49     F5IV-V 50 0
12 HD 179732 * 19 11 53.4817719639 +42 06 27.744947398   9.19 8.74     F5IV-V 34 0
13 HD 234856 Ro* 19 17 45.8021284617 +50 28 48.273320177   9.87 9.32     F9IV-V 65 0
14 HD 181207 PM* 19 17 46.3566541779 +41 24 36.837551319   9.06 8.47     F9IV-V 72 0
15 TYC 3555-1403-1 * 19 20 52.7237209312 +51 28 18.245887116   10.68 9.78     K0III-IV 24 0
16 BD+48 2882 Ro* 19 21 24.640392 +48 30 53.31924   10.27 9.45 9.36   G1V 44 0
17 BD+48 2887 * 19 22 20.2270265103 +48 41 43.494023410   9.43 9.01     F5IV 35 0
18 HD 183159 PM* 19 26 19.3089859132 +41 52 12.720359592   9.26 8.58     G1V 32 0
19 HD 183298 PM* 19 26 22.0908800928 +50 59 14.333199265   8.71 8.16     G0.5IV 76 0
20 BD+36 3570 Ro* 19 28 19.8470073047 +37 03 35.395152315   9.40 8.97     F8IV 49 0
21 TYC 3143-53-1 Ro* 19 35 03.7375425270 +42 44 16.720275774   10.31 9.85     F8IV 50 0
22 BD+44 3183 PM* 19 35 50.5740210502 +44 52 50.020113052   9.38 8.92     G0IV 46 0
23 KIC 11771760 * 19 43 57.7106783927 +49 55 21.497629035   12.02 11.89     G0 20 0
24 HD 234998 PM* 19 46 37.7416540232 +51 01 13.523892663   9.16 8.75     F5 32 0
25 HD 187160 SB* 19 46 41.3660194374 +44 20 54.685297711   7.650 7.083     F9IV-V 77 0
26 BD+47 2934 Ro* 19 50 14.2730383424 +47 28 25.164868973   9.68 9.24     F5IV-V 36 0
27 HD 188819 Ro* 19 54 54.1811994176 +47 08 42.947274296   9.12 8.66     F8IV 48 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2014A&A...566A..20A and select 'bookmark this link' or equivalent in the popup menu


2020.07.03-21:57:43

© Université de Strasbourg/CNRS

    • Contact