Numerical investigation of the stability of motion of a mass element ejected from a component of a binary star system

Details Numerical investigation of the stability of motion of a mass element ejected from a component of a binary star system Numerical investigation of the stability of motion of a mass element ejected from a component of a binary star system

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..283..123d&link_type=abstract

In: Mass-losing pulsating stars and their circumstellar matter. Workshop, May 13-16, 2002, Sendai, Japan, edited by Y. Nakada, M

Astronomy and Astrophysics

Astrophysics

Binaries, Celestial Dynamics, Circumstellar Matter, Numerical Integration, Numeriintegration

Scientific paper

The numerical investigation of the stability of motion of a mass element ejected from a component of a binary star system has been made. The small mass element is initially taken as rest and the binary components are assumed to be revolving in a circular orbit around the center of mass. Only planar motion has been considered. The stability of motion has been investigated using the Poincare surface of section method.

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