J/A+A/706/A311 RVs of 5 binaries with fast-rotating OB stars (Putkuri+, 2026)
Non-synchronous rotation in massive binary systems.
III. Characterizing five binary systems with fast-rotating OB stars.
Putkuri C., Gamen R., Morrell N.I., Benvenuto O.G., Ansin T., Arias J.I.,
Folatelli G., Bersten M.
<Astron. Astrophys. 706, A311 (2026)>
=2026A&A...706A.311P 2026A&A...706A.311P (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Stars, OB ; Radial velocities ;
Optical
Keywords: stars: fundamental parameters - stars: massive - stars: rotation
Abstract:
Among the binary systems discovered by the spectroscopic monitoring of
Southern Galactic O and WN stars, or the OWN Survey, several systems
exhibit very different line broadening between their components.
We aim to characterize these binary systems in order to understand the
causes behind their markedly different spectral line widths, providing
observational clues as to the physical mechanisms at play.
We used new and archival multi-epoch high-resolution optical spectra
for the radial velocity analysis and determined the spectroscopic
orbits of both components in five systems: HD 57236, HD 93028, HD
101413, HD 151003, and HD 153426. The physical properties of the
individual stellar components were determined through quantitative
analysis. Using evolutionary models, we estimated the age of the
systems and explored their tidal evolution.
The systems consist of O+O or O+B stars, with minimum masses ranging
from ∼6M☉ to 21M☉, in young, wide, and fairly eccentric
orbits (periods from approximately 22 to 977d and eccentricities of
e>0.14). The primary and secondary components have a projected
rotational velocity ratio of up to 1:7 (∼27 and ∼193km/s in
the case of HD 93028), similar to previous binary systems in this
series, namely HD 93343 and HD 96264A.
The youth and wide orbits of the systems indicate that the
non-synchronous rotational nature of their components is a consequence
of the stellar formation process, rather than a result of past binary
interactions. While the role of binary interactions may be predominant
in many cases, it is not a necessary condition to explain the entire
observed population of fast rotators.
Description:
The orbital phase (Phase) was computed according to the ephemerides of
the orbital solution presented in Table 2. The typical
uncertainties in the RVs are 3 and 10km/s, for the narrow and broad
components, respectively.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 35 5 List of studied stars
appena.dat 41 231 Radial velocity measurements for the 5 systems
(tables A1-A5)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: stars.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Star Star name
13- 14 I2 h RAh Simbad right ascension (J2000)
16- 17 I2 min RAm Simbad right ascension (J2000)
19- 23 F5.2 s RAs Simbad right ascension (J2000)
25 A1 --- DE- Simbad declination sign (J2000)
26- 27 I2 deg DEd Simbad declination (J2000)
29- 30 I2 arcmin DEm Simbad declination (J2000)
32- 35 F4.1 arcsec DEs Simbad declination (J2000)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: appena.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Star Star name
11- 21 F11.3 d HJD Heliocentric Julian Date of the observation
24- 28 F5.3 --- Phase Orbital phase
30- 32 I3 km/s RV1 Radial velocity of the primary component
34- 37 I4 km/s RV2 ? Radial velocity of the secondary component
39- 41 A3 --- Obs Observatory where the spectrum was obtained
--------------------------------------------------------------------------------
Acknowledgements:
Cristina Putkuri, cristyfisic(at)gmail.com
References:
Putkuri et al., Paper I 2018A&A...618A.174P 2018A&A...618A.174P
Putkuri et al., Paper II 2021A&A...650A..96P 2021A&A...650A..96P
(End) Patricia Vannier [CDS] 09-Jan-2026