2014A&A...566A..82L


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.14CEST02:08:51

2014A&A...566A..82L - Astronomy and Astrophysics, volume 566A, 82-82 (2014/6-1)

AME - Asteroseismology Made Easy. Estimating stellar properties by using scaled models.

LUNDKVIST M., KJELDSEN H. and SILVA AGUIRRE V.

Abstract (from CDS):

Stellar properties and, in particular stellar radii of exoplanet host stars, are essential for measuring the properties of exoplanets, therefore it is becoming increasingly important to be able to supply reliable stellar radii fast. Grid-modelling is an obvious choice for this, but that only offers a low degree of transparency to non-specialists. Here we present a new, easy, fast, and transparent method of obtaining stellar properties for stars exhibiting solar-like oscillations. The method, called Asteroseismology Made Easy (AME), can determine stellar masses, mean densities, radii, and surface gravities, as well as estimate ages. We present AME as a visual and powerful tool that could be useful, in particular, in light of the large number of exoplanets being found. AME consists of a set of figures from which the stellar parameters can be deduced. These figures are made from a grid of stellar evolutionary models that cover masses ranging from 0.7M to 1.6M in steps of 0.1M and metallicities in the interval -0.3dex≤[Fe/H]≤+0.3dex in increments of 0.1dex. The stellar evolutionary models are computed using the Modules for Experiments in Stellar Astrophysics (MESA) code with simple input physics. We have compared the results from AME with results for three groups of stars: stars with radii determined from interferometry (and measured parallaxes), stars with radii determined from measurements of their parallaxes (and calculated angular diameters), and stars with results based on modelling their individual oscillation frequencies. We find that a comparison of the radii from interferometry to those from AME yields a weighted mean of the fractional differences of just 2%. This is also the level of deviation that we find when we compare the parallax-based radii to the radii determined from AME. The comparison between independently determined stellar parameters and those found using AME show that our method can provide reliable stellar masses, radii, and ages, with median uncertainties in the order of 4%, 2%, and 25%, respectively.

Abstract Copyright:

Journal keyword(s): asteroseismology - stars: fundamental parameters - stars: low-mass - stars: solar-type

Simbad objects: 41

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Number of rows : 41

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 * bet Hyi PM* 00 25 45.07036 -77 15 15.2860 3.52 3.41 2.79 2.28 1.94 G0V 528 0
2 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1739 0
3 SA 12- reg 08 48 +09.5           ~ 4 0
4 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3882 3
5 NAME Cen B QSO 13 46 49.04327124 -60 24 29.3552337         15.74 ~ 120 0
6 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 646 1
7 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 863 1
8 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1106 0
9 * mu. Ara PM* 17 44 08.7036342277 -51 50 02.591049123   5.85 5.15     G3IV-V 454 2
10 HD 173701 PM* 18 44 35.1192273920 +43 49 59.789089625   8.37 7.52     G8V 120 0
11 HD 175226 * 18 52 16.4987183752 +43 42 35.795775824   7.91 7.42     F6IV 49 0
12 KOI-245 Ro* 18 56 14.3077765754 +44 31 05.389239372   10.45 9.77     ~ 89 4
13 BD+45 2796 PM* 18 56 21.2644967292 +45 30 53.232987726   9.80 9.29     G0.5IV 61 0
14 HD 176071 PM* 18 56 22.1269692202 +45 30 25.359126300   8.81 8.33     F8IV 60 0
15 HD 176153 Ro* 18 56 36.6478619140 +47 39 23.163197712   9.20 8.68     F9IV-V 60 0
16 HD 177153 PM* 19 01 39.6781881955 +41 29 24.325583971   7.76 7.21     G0 82 0
17 Kepler-10 Ro* 19 02 43.0612302512 +50 14 28.700759378       11.00   G 145 4
18 HD 177723 * 19 03 45.1359001568 +45 36 30.188777836   9.54 9.10     F8IV 42 0
19 HD 177780 * 19 04 16.3774387772 +41 00 11.443194845   9.01 8.37     G3V 29 0
20 HD 178971 Ro* 19 09 01.9440013031 +38 53 59.483977067   8.79 8.36     F5IV-V 48 0
21 HD 179070 Ro* 19 09 26.8351401260 +38 42 50.455094310   8.767 8.25 8.00   F6IV 126 3
22 KOI-262 Ro* 19 12 24.2129932892 +50 02 01.370843497   11.02 10.54     F5 82 3
23 KOI-97 Er* 19 14 19.5623271934 +41 05 23.365460942           G0 91 3
24 KOI-85 Ro* 19 14 45.2919793492 +41 09 04.207327203   11.62 10.92     F6IV 77 1
25 HD 180867 * 19 15 54.6869420707 +47 03 40.229155655   8.75 8.24     F6IV 46 0
26 BD+39 3706 PM* 19 16 34.9029087477 +40 02 50.362111184       9.1   G1.5V 56 0
27 HD 234856 Ro* 19 17 45.8021284617 +50 28 48.273320177   9.87 9.32     F9IV-V 62 0
28 BD+43 3209 * 19 18 54.1341967279 +43 29 46.690440128   10.14 9.52 9.46   F9IV-V 27 0
29 BD+43 3221 * 19 20 47.9394314405 +44 09 18.749657280   10.03 9.50     F9IV-V 53 0
30 HD 182736 Er* 19 24 03.3794425774 +44 56 00.735214599   7.82 7.01     G8IV 57 0
31 KOI-246 * 19 24 07.7660110490 +49 02 24.928201112   10.73 10.08     ~ 83 5
32 KOI-277 Ro* 19 25 00.0430855076 +49 13 54.631289830   12.66 11.94     ~ 150 3
33 HD 183298 PM* 19 26 22.0908800928 +50 59 14.333199265   8.71 8.16     G0.5IV 71 0
34 BD+47 2846 Er* 19 28 59.3538131541 +47 58 10.216250846   10.97 10.48     F6V 240 2
35 * tet Cyg PM* 19 36 26.5343563 +50 13 15.964573 4.83 4.86 4.48 4.13 3.92 F3+V 320 1
36 HD 185457 * 19 37 27.6975906190 +40 35 19.911599371   8.93 8.42     F8IV 29 0
37 * 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
38 * 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
39 HD 186700 PM* 19 43 39.6224377398 +48 55 43.808257365   8.86 8.47     F5IV-V 51 0
40 HD 187637 PM* 19 49 18.1388420406 +41 34 56.857643338       7.2   F8V 80 0
41 HD 188819 Ro* 19 54 54.1811994176 +47 08 42.947274296   9.12 8.66     F8IV 45 0

    Equat.    Gal    SGal    Ecl

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2019.10.14-02:08:51

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