J/A+A/671/A139 Four high-mass eclipsing binaries light curves (Pavlovski+, 2023)
High-mass eclipsing binaries: A testbed for models of interior structure and
evolution. Accurate fundamental properties and surface chemical composition for
V1034 Sco, GL Car, V573 Car and V346 Cen.
Pavlovski K., Southworth J., Tkachenko A., Van Reeth A., Tamajo E.
<Astron. Astrophys. 671, A139 (2023)>
=2023A&A...671A.139P 2023A&A...671A.139P (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Photometry ; Optical
Keywords: stars: fundamental parameters - stars: evolution -
binaries: spectroscopic - binaries: eclipsing - stars: abundances
Abstract:
The surface chemical compositions of stars are affected by physical
processes which bring the products of thermonuclear burning to the
surface. Despite their potential in understanding the structure and
evolution of stars, elemental abundances are available for only a few
high-mass binary stars. We aim to enlarge this sample by determining
the physical properties and photospheric abundances for four eclipsing
binary systems containing high-mass stars: V1034 Sco, GL Car, V573 Car
and V346 Cen. The components have masses 8 too 17M☉ and effective
temperatures from 22500 to 32200K, and are all on the main sequence.
We present new high-resolution and high signal-to-noise spectroscopy
from High Accuracy Radial velocity Planet Searcher (HARPS), and
analyse them using spectral disentangling and non-local thermodynamic
equilibrium (NLTE) spectral synthesis. We model existing light curves
and new photometry from the Transiting Exoplanet Survey Satellite
(TESS).
We measure the stellar masses to 0.6 to 2.0% precision, radii to 0.8
to 1.7% precision, effective temperatures to 1.1 to 1.6% precision,
and abundances of C, N, O, Mg and Si. The abundances are similar to
those found in our previous studies of high-mass eclipsing binaries;
our sample now comprises 25 high-mass stars in 13 binary systems. We
also find tidally-excited pulsations in V346 Cen.
We reinforce our previous conclusions: interior chemical element
transport is not as efficient in binary star components as in their
single-star counterparts in the same mass regime and evolutionary
stage, possibly due to the effects of tidal forces. Our ultimate goal
is to provide a larger sample of OB-type stars in binaries which would
enable a thorough comparison to stellar evolutionary models, as well
as to single high-mass stars.
Description:
Light curves measured from the full frame images (FFIs) of the
Transiting Exoplanet Space Satellite (TESS) were obtained and used in
the determination of the physical properties of the high-mass
eclipsing binaries V1034 Sco, GL Car, V573 Car and V346 Cen.
Objects:
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RA (2000) DE Designation(s)
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16 54 19.83 -41 50 09.3 V1034 Sco = TIC 339568071
11 14 39.83 -60 39 36.3 GL Car = HD 306168
10 45 08.22 -59 40 49.4 V573 Car = TIC 458859930
11 42 49.67 -62 26 05.4 V346 Cen = TIC 322079159
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 75 4 Basic characteristics of the binary systems
studied in this work
tablea1.dat 35 28927 Differential photometry of the target eclipsing
binaries from TESS
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See also:
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Target GCVS name of the target eclipsing binary
11- 21 A11 --- OName Other name
23- 26 F4.2 d Porb Orbital period
28- 31 F4.2 mag Vmax Maximum V magnitude
33- 47 A15 --- SpType Spectral types
49- 52 A4 Myr Age Age
53- 63 A11 --- Memb Cluster membership
65- 70 F6.2 yr Paps ?=- Apsidal period
72- 75 F4.2 yr e_Paps ? Apsidal period error
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Target GCVS name of the target eclipsing binary
11- 12 I2 --- Sector TESS sector the measurement was obtained during
14- 26 F13.5 d BJD Barycentric Julian Date for the midpoint of
observation (TDB)
28- 35 F8.5 mag mag Differential TESS-band magnitude
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Acknowledgements:
John Southworth, taylorsouthworth(at)gmail.com
(End) John Southworth [Keele Univ., UK], Patricia Vannier [CDS] 09-Feb-2023