Volume 618, October 2018
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||26 October 2018|
Non-synchronous rotations in massive binary systems
HD 93343 revisited⋆
Instituto de Astrofísica de La Plata (CONICET-UNLP), Paseo del Bosque s/n, 1900 La Plata, Argentina
2 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
3 Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
4 Instituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Spain
5 Departamento de Astrofísica, Universidad de La Laguna, 38205, La Laguna Tenerife, Spain
6 Departamento de Física y Astronomía, Universidad de La Serena, Av. Cisternas 1200 Norte, La Serena, Chile
Accepted: 22 July 2018
Context. Most massive stars are in binary or multiple systems. Several massive stars have been detected as double-lined spectroscopic binaries and among these, the OWN Survey has detected a non-negligible number whose components show very different spectral line broadening (i.e., projected rotational velocities). This fact raises a discussion about the contributing processes, such as angular-momentum transfer and tidal forces.
Aims. We seek to constrain the physical and evolutionary status of one of such systems, the O+O binary HD 93343.
Methods. We analyzed a series of high-resolution multiepoch optical spectra to determine the orbital parameters, projected rotational velocities, and evolutionary status of the system.
Results. HD 93343 is a binary system comprised of two O7.5 Vz stars that each have minimum masses of approximately 22 M⊙ in a wide and eccentric orbit (e = 0.398±0.004; P = 50.432±0.001 d). Both stars have very similar stellar parameters, and hence ages. As expected from the qualitative appearance of the combined spectrum of the system, however, these stars have very different projected rotational velocities (~65 and ~325 km s−1, respectively).
Conclusions. The orbits and stellar parameters obtained for both components seem to indicate that their youth and relative separation is enough to discard the effects of mass transfer and tidal friction. Thus, non-synchronization should be intrinsic to their formation.
Key words: binaries: spectroscopic / stars: early-type / stars: rotation / stars: individual: HD 93343
© ESO 2018
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