2017A&A...598A..74P


Query : 2017A&A...598A..74P

2017A&A...598A..74P - Astronomy and Astrophysics, volume 598A, 74-74 (2017/2-1)

Signatures of internal rotation discovered in the Kepler data of five slowly pulsating B stars.

PAPICS P.I., TKACHENKO A., VAN REETH T., AERTS C., MORAVVEJI E., VAN DE SANDE M., DE SMEDT K., BLOEMEN S., SOUTHWORTH J., DEBOSSCHER J., NIEMCZURA E. and GAMEIRO J.F.

Abstract (from CDS):

Context. Massive stars are important building blocks of the Universe, and their stellar structure and evolution models are fundamental cornerstones of various fields in modern astrophysics. The precision of these models is strongly limited by our lack of understanding of various internal mixing processes that significantly influence the lifetime of these objects, such as core overshoot, chemical mixing, or the internal differential rotation.
Aims. Our goal is to calibrate models by extending the sample of available seismic studies of slowly pulsating B (SPB) stars, providing input for theoretical modelling efforts that will deliver precise constraints on the parameters describing the internal mixing processes in these objects.
Methods. We used spectral synthesis and disentangling techniques to derive fundamental parameters and to determine precise orbital parameters from high-resolution spectra. We employed custom masks to construct light curves from the virtually uninterrupted four year long Kepler pixel data and used standard time-series analysis tools to construct a set of significant frequencies for each target. These sets were first filtered from combination frequencies, and then screened for period spacing patterns.
Results. We detect gravity mode period series of modes, of the same degree l with consecutive radial order n, in four new and one revisited SPB star. These series (covering typically 10 to 40 radial orders) are clearly influenced by moderate to fast rotation and carry signatures of chemical mixing processes. Furthermore, they are predominantly prograde dipole series. Our spectroscopic analysis, in addition to placing each object inside the SPB instability strip and identifying KIC 4930889 as an SB2 binary, reveals that KIC 11971405 is a fast rotator that shows very weak Be signatures. Together with the observed photometric outbursts this illustrates that this Be star is a fast rotating SPB star. We hypothesise that the outbursts might be connected to its very densely compressed oscillation spectrum.

Abstract Copyright: © ESO, 2017

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

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 HD 43317 Pu* 06 15 47.0134228488 +04 17 01.095049500 5.82 6.456 6.614     B3IV 114 0
2 HD 46179 ** 06 32 07.1393096040 +06 02 08.278506528   6.659 6.706     B9V 37 0
3 * 16 Mon SB* 06 46 32.4145190352 +08 35 13.767386136   5.76 5.92     B3V 95 0
4 HD 49330 bC* 06 47 57.2679459720 +00 46 34.035384504 8.45 9.14 8.95     Bnn(e) 89 0
5 HD 50230 Pu* 06 52 19.8143879448 -00 40 38.959876308   8.93 8.95     B3III 51 0
6 HD 50846 EB* 06 54 54.7081653504 -01 22 32.850081768   8.46 8.43     B5/7Ib 149 0
7 * ome CMa Be* 07 14 48.6538664 -26 46 21.609714 2.90 3.64 3.82 3.80 3.90 B2.5Ve 352 0
8 HD 174648 * 18 51 41.0002474368 -01 45 35.238378132   8.90 8.81     B9.5V 20 0
9 HD 174884 EB* 18 52 40.3063548312 +04 03 11.755214640   8.14 7.998     B8V 39 0
10 HD 179506 Ro* 19 10 57.7607883552 +41 46 33.421683180   7.87 7.91     B8VsHestr(B6) 40 0
11 2MASS J19120273+4742364 Pu* 19 12 02.7395758512 +47 42 36.406192932           B8.3V 63 0
12 * d Aql * 19 20 35.6863700904 -00 53 31.774520544 5.22 5.408 5.451     B9III 54 0
13 HD 182198 * 19 23 31.6234725264 -00 32 26.093724108   8.10 7.94     B9III 19 0
14 2MASS J19253699+4523448 Ro* 19 25 36.9899720424 +45 23 44.902125744           ~ 16 0
15 HD 184939 SB* 19 35 07.8332799936 +40 01 28.891242084   8.79 8.86     A2 25 0
16 TYC 3139-291-1 Pu* 19 36 00.8890646712 +40 05 55.052761308   11.52 11.37     B8III 13 0
17 BD+43 3310 Pu* 19 37 29.7688619736 +43 24 57.369736800   10.32 10.28     B9IV 52 0
18 2MASS J19405445+3834503 Pu* 19 40 54.4541104248 +38 34 50.348300448           B6.5IV 20 0
19 HD 186567 Ro* 19 42 48.8430567072 +50 21 39.806399160   9.07 9.21   9.191 F 28 0

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