Bibcode
Simón-Díaz, S.; Caballero, J. A.; Lorenzo, J.
Bibliographical reference
The Astrophysical Journal, Volume 742, Issue 1, article id. 55 (2011).
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11
2011
Journal
Citations
28
Refereed citations
22
Description
We report on the detection of a third massive star component in the
σ Orionis AB system, traditionally considered as a binary system.
The system has been monitored by the IACOB Spectroscopic Survey of
Northern Massive Stars program, obtaining 23 high-resolution FIES@NOT
spectra with a time span of ~2.5 years. The analysis of the radial
velocity curves of the two spectroscopic components observed in the
spectra has allowed us to obtain the orbital parameters of the system,
resulting in a high eccentric orbit (e ~ 0.78) with an orbital period of
143.5 ± 0.5 days. This result implies the actual presence of
three stars in the σ Orionis AB system when combined with previous
results obtained from the study of the astrometric orbit (with an
estimated period of ~157 years).
Based on observations made with the Nordic Optical Telescope, operated
on the island of La Palma jointly by Denmark, Finland, Iceland, Norway,
and Sweden, in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias.
Related projects
Physical properties and evolution of Massive Stars
This project aims at the searching, observation and analysis of massive stars in nearby galaxies to provide a solid empirical ground to understand their physical properties as a function of those key parameters that gobern their evolution (i.e. mass, spin, metallicity, mass loss, and binary interaction). Massive stars are central objects to
Sergio
Simón Díaz