2014A&A...570A...8P


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST19:44:15

2014A&A...570A...8P - Astronomy and Astrophysics, volume 570A, 8-8 (2014/10-1)

KIC 10526294: a slowly rotating B star with rotationally split, quasi-equally spaced gravity modes.

PAPICS P.I., MORAVVEJI E., AERTS C., TKACHENKO A., TRIANA S.A., BLOEMEN S. and SOUTHWORTH J.

Abstract (from CDS):

Massive stars are important for the chemical enrichment of the universe. Since internal mixing processes influence their lives, it is very important to place constraints on the corresponding physical parameters, such as core overshooting and the internal rotation profile, so as to calibrate their stellar structure and evolution models. Although asteroseismology has been shown to be able to deliver the most precise constraints so far, the number of detailed seismic studies delivering quantitative results is limited. Our goal is to extend this limited sample with an in-depth case study and provide a well-constrained set of asteroseismic parameters, contributing to the ongoing mapping efforts of the instability strips of the β Cep and slowly pulsating B (SPB) stars. We derived fundamental parameters from high-resolution spectra using spectral synthesis techniques. We used custom masks to obtain optimal light curves from the original pixel level data from the Kepler satellite. We used standard time-series analysis tools to construct a set of significant pulsation modes that provide the basis for the seismic analysis carried out afterwards.We find that KIC10526294 is a cool SPB star, one of the slowest rotators ever found. Despite this, the length of Kepler observations is sufficient to resolve narrow rotationally split multiplets for each of its nineteen quasi-equally spaced dipole modes. The number of detected consecutive (in radial order) dipole modes in this series is higher than ever before. The observed amount of splitting shows an increasing trend towards longer periods, which - largely independent of the seismically calibrated stellar models - points towards a non-rigid internal rotation profile. From the average splitting we deduce a rotation period of ∼188 days. From seismic modelling, we find that the star is young with a central hydrogen mass fraction Xc>0.64; it has a core overshooting αov≤0.15.

Abstract Copyright:

Journal keyword(s): asteroseismology - stars: variables: general - stars: early-type - stars: fundamental parameters - stars: oscillations - stars: rotation

Errata: + corrigendum vol. 570, p. C4

Simbad objects: 14

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Number of rows : 14

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 HD 43317 Pu* 06 15 47.0136233779 +04 17 01.097508973 5.82 6.456 6.614     B3IV 85 0
2 HD 46179 ** 06 32 07.1392982683 +06 02 08.289835111   6.659 6.706     B9V 31 0
3 * 16 Mon SB* 06 46 32.4144659902 +08 35 13.781782532   5.76 5.92     B3V 86 0
4 HD 50230 Pu* 06 52 19.8149287598 -00 40 38.956577604   8.93 8.95     B3III 43 0
5 HD 50846 Al* 06 54 54.7083961175 -01 22 32.849416553   8.46 8.43     B5/7Ib 132 0
6 HD 174648 * 18 51 41.0001981972 -01 45 35.240841550   8.90 8.81     B9.5V 13 0
7 HD 174884 SB* 18 52 40.3070448846 +04 03 11.737986016   8.14 7.998     B8V 27 0
8 HD 179506 Ro* 19 10 57.7592001776 +41 46 33.451401349   7.87 7.91     B8VsHestr(B6) 24 0
9 KIC 10526294 Pu* 19 12 02.7398748040 +47 42 36.408857134           B8.3V 46 0
10 * d Aql * 19 20 35.6861889272 -00 53 31.783617753 5.22 5.408 5.451     B9III 47 0
11 HD 181558 Pu* 19 21 37.1136252032 -19 14 04.049964502 5.65 6.16 6.26     B5III 60 0
12 HD 182198 * 19 23 31.6234958461 -00 32 26.092830977   8.10 7.94     B9III 14 0
13 TYC 3139-291-1 Pu* 19 36 00.8891030892 +40 05 55.052844235   11.52 11.37     B8III 13 0
14 KIC 11145123 dS* 19 41 25.3412172674 +48 45 14.989333768           A 22 0

    Equat.    Gal    SGal    Ecl

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2019.10.20-19:44:15

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