Bibcode
Simón-Díaz, S.; Caballero, J. A.; Lorenzo, J.
Referencia bibliográfica
The Astrophysical Journal, Volume 742, Issue 1, article id. 55 (2011).
Fecha de publicación:
11
2011
Revista
Número de citas
28
Número de citas referidas
22
Descripción
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.
Proyectos relacionados
Propiedades Físicas y Evolución de Estrellas Masivas
Las estrellas masivas son objetos claves para la Astrofísica. Estas estrellas nacen con más de 8 masas solares, lo que las condena a morir como Supernovas. Durante su rápida evolución liberan, a través de fuertes vientos estelares, gran cantidad de material procesado en su núcleo y, en determinadas fases evolutivas, emiten gran cantidad de
Sergio
Simón Díaz