Tidally induced mass loss in IOTA Orionis

Details Tidally induced mass loss in IOTA Orionis Tidally induced mass loss in IOTA Orionis

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986esasp.263..487s&link_type=abstract

In ESA Proceedings of an International Symposium on New Insights in Astrophysics. Eight Years of UV Astronomy with IUE p 487-49

Astronomy and Astrophysics

Astrophysics

1

Binary Stars, Stellar Mass Ejection, Stellar Spectrophotometry, Iue, Stellar Spectra, Stellar Winds, Ultraviolet Spectroscopy

Scientific paper

Mass loss in Iota Orionis, a massive O9 III + B1 III binary with a highly eccentric orbit was investigated. Coude spectra from RGO were used to update its ephemeris and establish a value for the apsidal motion. Combining the orbital elements, the astrophysical data (the primary is an O9 III standard star in the Orion Association), and photometry through a grazing eclipse the dimensions of the system were determined. This shows that at periastron, the centers of the stars are only separated by 1.5 times the sum of the radii, which suggests that strong tidal forces are generated and enhanced mass loss may be expected. Evidence of this was sought in high resolution IUE spectra taken through periastron passage: perturbations of the wind lines of C IV, N V and Si IV are seen.

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