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Line-Profile Variations on Massive Binary Systems: Determining η Carinae Orbital Parameters

Published online by Cambridge University Press:  12 July 2007

D. Falceta-Gonçalves ,
Z. Abraham  and
V. Jatenco-Pereira
D. Falceta-Gonçalves
Affiliation:
Instituto de Astronomia, Universidade de São Paulo, Rua do Matão 1226, CEP 05508-900, São Paulo, Brazil email: [email protected]
Z. Abraham
Affiliation:
Instituto de Astronomia, Universidade de São Paulo, Rua do Matão 1226, CEP 05508-900, São Paulo, Brazil email: [email protected]
V. Jatenco-Pereira
Affiliation:
Instituto de Astronomia, Universidade de São Paulo, Rua do Matão 1226, CEP 05508-900, São Paulo, Brazil email: [email protected]
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Abstract

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When the winds of two massive stars orbiting each other collide, an interaction zone is created consisting of two shock fronts at both sides of a contact surface. During the cooling process, elements may recombine generating spectral lines. These lines may be Doppler shifted, as the gas stream flows over the interaction zone. To calculate the stream velocity projected into the line of sight we use a simplified conical geometry for the shock fronts and, to determine the synthetic line profile, we have to sum the amount of emitting gas elements with the same Doppler shifted velocity. We show that the stellar mass loss rates and wind velocities, and the orbital inclination and eccentricity, are the main parameters on this physical process. By comparing observational data to the synthetic line profiles it is possible to determine these parameters. We tested this process to Brey 22 WR binary system, and applied to the enigmatic object of η Carinae.

Keywords

binaries: generalWolf-Rayetwindsline: profiles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S240: Binary Stars as Critical Tools & Tests in Contemporary Astrophysics , August 2006 , pp. 198 - 201
Copyright
Copyright © International Astronomical Union 2007

References

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