2019A&A...624A..35K


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.03CET19:36:10

2019A&A...624A..35K - Astronomy and Astrophysics, volume 624A, 35-35 (2019/4-1)

Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE-Constellation.

KALLINGER T., BECK P.G., HEKKER S., HUBER D., KUSCHNIG R., ROCKENBAUER M., WINTER P.M., WEISS W.W., HANDLER G., MOFFAT A.F.J., PIGULSKI A., POPOWICZ A., WADE G.A. and ZWINTZ K.

Abstract (from CDS):


Context. The study of stellar structure and evolution depends crucially on accurate stellar parameters. The photometry from space telescopes has provided superb data that enabled the asteroseismic characterisation of thousands of stars. However, typical targets of space telescopes are rather faint and complementary measurements are difficult to obtain. On the other hand, the brightest, otherwise well-studied stars, are lacking seismic characterization.
Aims. Our goal is to use the granulation and/or oscillation timescales measured from photometric time series of bright red giants (1.6≤Vmag≤5.3) observed with BRITE-Constellation to determine stellar surface gravities and masses.
Methods. We used probabilistic methods to characterise the granulation and/or oscillation signal in the power density spectra and the autocorrelation function of the BRITE-Constellation time series.
Results. We detect a clear granulation and/or oscillation signal in 23 red giant stars and extract the corresponding timescales from the power density spectra as well as the autocorrelation function of the BRITE-Constellation time series. To account for the recently discovered non-linearity of the classical seismic scaling relations, we used parameters from a large sample of Kepler stars to re-calibrate the scalings of the high- and low-frequency components of the granulation signal. We developed a method to identify which component is measured if only one granulation component is statistically significant in the data. We then used the new scalings to determine the surface gravity of our sample stars, finding them to be consistent with those determined from the autocorrelation signal of the time series. We further used radius estimates from the literature to determine the stellar masses of our sample stars from the measured surface gravities. We also defined a statistical measure for the evolutionary stage of the stars.
Conclusions. Our sample of stars covers low-mass stars on the lower giant branch to evolved massive supergiants and even though we cannot verify our mass estimates with independent measurements from the literature, they appear to be at least good enough to separate high-mass from low-mass stars. Given the large known but usually not considered systematic uncertainties in the previous model-based mass estimates, we prefer our model-independent measurements.

Abstract Copyright: © ESO 2019

Journal keyword(s): stars: fundamental parameters - stars: oscillations - stars: interiors

Simbad objects: 30

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Number of rows : 30

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 Ass Per OB 1 As* 02 21 +57.6           ~ 162 1
2 NAME Cet I GrG 02 28.2 -01 21           ~ 8 0
3 * alf Cet LP? 03 02 16.77307 +04 05 23.0596 6.10 4.17 2.53 1.18 0.02 M1.5IIIa 440 0
4 * rho Per LP* 03 05 10.59385 +38 50 24.9943 6.83 5.04 3.39 1.59 -0.03 M4+IIIa 307 0
5 HD 19349 * 03 06 33.4936866467 -06 05 18.763459019   6.808 5.256     M2/3II 38 0
6 * sig Per V* 03 30 34.4872784580 +47 59 42.780422381 7.25 5.71 4.36     K3-III 117 0
7 * sig CMa LP* 07 01 43.1477846 -27 56 05.389774 7.08 5.20 3.47 2.15 1.15 K5Ib 166 0
8 * h01 Pup LP* 08 11 21.4922571895 -39 37 06.766597581 7.79 6.03 4.42 3.22 2.34 K4.5Ib 55 0
9 * bet Pyx * 08 40 06.1436306 -35 18 30.065139   4.885 3.954     G5II/III 67 0
10 * g Car V* 09 16 12.0728569 -57 32 29.300662   5.941 4.318     M0.5IIIa 33 0
11 * N Vel V* 09 31 13.3189137 -57 02 03.757780   4.691 3.139     K5III 89 0
12 * q Car LP* 10 17 04.9753050 -61 19 56.288301   4.899 3.350     K2.5II 126 0
13 V* GZ Vel LP* 10 19 36.7507384 -55 01 45.502292   6.146 4.543     K2.5II 51 0
14 NAME Carina I HII Region HII 10 43 32 -59 35.0           ~ 51 0
15 * 12 Mus RS* 11 39 29.59368 -65 23 51.9586   5.863 5.095 6.31   G5/8IIIp+A0/1V 155 1
16 * eps Mus LP* 12 17 34.2771607 -67 57 38.648630 7.27 5.60 4.02 2.12 0.36 M4III 68 0
17 * eps Cru PM* 12 21 21.6093625 -60 24 04.129070   5.01 3.59     K3III 83 0
18 * gam Cru PM* 12 31 09.95961 -57 06 47.5684 5.01 3.23 1.64 -0.02 -1.44 M3.5III 264 0
19 * eps Sco PM* 16 50 09.8108127 -34 17 35.633735 4.61 3.45 2.29 1.43 0.83 K1III 201 0
20 * G Sco * 17 49 51.4808134 -37 02 35.897520 5.57 4.38 3.21     K2III 74 0
21 * eta Sgr LP? 18 17 37.6350518 -36 45 42.066723 6.37 4.67 3.11 1.55 0.23 M2III 133 0
22 KIC 1431599 RG* 19 25 01.1657281715 +37 05 11.149642254           ~ 2 0
23 NAME Laevens 5 Gl? 19 52 40.5 -22 04 05           ~ 35 0
24 * eta Cyg * 19 56 18.3722223 +35 05 00.322759 5.800 4.910 3.880 3.19 2.66 K0III 270 0
25 NAME Bubble around HD 191765 HI 20 10 +36.1           ~ 7 0
26 * 23 Vul ** 20 15 46.1444650590 +27 48 51.099784408 6.89 5.78 4.52 3.56 2.85 K3-IIIFe-1 107 1
27 * 39 Cyg SB* 20 23 51.6206989 +32 11 24.619097 7.27 5.77 4.44 3.43 2.76 K2.5IIIFe-0.5 131 0
28 * eps Cyg ** 20 46 12.6823609 +33 58 12.924926 4.370 3.520 2.480 1.73 1.19 K0III 481 0
29 NAME Eri I ~ ~ ~           ~ 3 0
30 NAME PUP I assoc Cl* ~ ~           ~ 3 0

    Equat.    Gal    SGal    Ecl

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2020.12.03-19:36:10

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