Trajectories and envelopes in the repulsive two-fixed-centre problem and in the restricted three-body problem

Details Trajectories and envelopes in the repulsive two-fixed-centre problem and in the restricted three-body problem Trajectories and envelopes in the repulsive two-fixed-centre problem and in the restricted three-body problem

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992cemda..53...37k&link_type=abstract

Celestial Mechanics and Dynamical Astronomy (ISSN 0923-2958), vol. 53, no. 1, 1992, p. 37-57. Research supported by Cusanuswerk

Astronomy and Astrophysics

Astronomy

4

Binary Stars, Particle Trajectories, Stellar Envelopes, Stellar Models, Stellar Winds, Three Body Problem, Centrifugal Force, Coriolis Effect, Elliptic Functions, Isoenergetic Processes, Supersonic Flow, Weierstrass Functions

Scientific paper

The envelope of iso-energetic trajectories in the (repulsive) two-fixed-center problem is derived. Analytical calculations finally lead to a transcendental equation, only containing elliptic integrals and the Weierstrass function, from which the envelope is constructed. The results may serve as a simple model for the boundary layer between two colliding supersonic stellar wind flows in binary systems, in which at least one of the components has a strong radiation field. Beyond this, the effect of noninertial forces due to the binary's orbital motion has been estimated by a numerical analysis within the scope of the (repulsive) restricted three-body problem. All calculations have been performed for a hot model (Wolf-Rayet/O-star) binary system with a set of parameters which might be appropriate for HD 152270.

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