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Shock structures in stellar winds resulting from orbital motions of the star

Published online by Cambridge University Press:  25 May 2016

Jorge Cantó ,
Alejandro Raga ,
Gloria Koenigsberger  and
Edmundo Moreno
Jorge Cantó
Affiliation:
Instituto de Astronomía, UNAM, Ap. 70–264, 04510 D.F., México
Alejandro Raga
Affiliation:
Instituto de Astronomía, UNAM, Ap. 70–264, 04510 D.F., México
Gloria Koenigsberger
Affiliation:
Instituto de Astronomía, UNAM, Ap. 70–264, 04510 D.F., México
Edmundo Moreno
Affiliation:
Instituto de Astronomía, UNAM, Ap. 70–264, 04510 D.F., México

Abstract

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We study the problem of a wind ejected from a star which orbits around a (wind-less) companion star. The orbital motion induces the formation of a spiral shock structure in the wind. An analytic formulation of the problem allows us to obtain the distance from the star at which the shock waves appear, and also the locus of the spiral, two-shock structure (i.e., the working surface). The full, three-dimensional structure of the working surface is found to have a spiral intersection with the orbital plane, and a cylindrical “hole” around the polar axis.

Type
Part 3. Interaction of Wolf-Rayet stars and other hot massive stars with their environment: colliding winds and ring nebulae
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 338 - 339
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Cantó, J., Raga, A.C., D'Alessio, P. 1999, MNRAS submitted.Google Scholar