The early-type multiple system Eta Orionis. I - Photometric variability and rediscussion of the physical parameters of the components

Details The early-type multiple system Eta Orionis. I - Photometric variability and rediscussion of the physical parameters of the components The early-type multiple system Eta Orionis. I - Photometric variability and rediscussion of the physical parameters of the components

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...194..143w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 194, no. 1-2, April 1988, p. 143-152.

Astronomy and Astrophysics

Astrophysics

10

Binary Stars, Early Stars, Stellar Mass, Stellar Spectrophotometry, Variable Stars, Light Curve, Radial Velocity

Scientific paper

The authors have studied the photometric variability of the multiple early B star η Orionis AabcB during the eclipses of the Aab pair and outside eclipse. They have determined that the short orbital period is 7.989255±0.000005 days, the primary and secondary eclipses are 0.24 mag and 0.23 mag deep, respectively. The period of the rapid variation is 0.43208±0.00001 days, and the integrated amplitude is 0.057 mag. The η Orionis system, which contains a visual triple, a spectroscopic triple, and a totally eclipsing pair, offers an exceptional opportunity for determining physical parameters of massive stars. A new value of 9.51 yr is proposed for the orbital period of the Aab, c system. The most likely model is that component B is itself a close binary, but this model is not supported by a comparison with other stars with similar variations. The possibility is then explored that variables of this kind are single rapidly rotating objects with triaxial ellipsoidal configurations.

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