Angular momentum loss and mass-exchange instability in binary stars

Details Angular momentum loss and mass-exchange instability in binary stars Angular momentum loss and mass-exchange instability in binary stars

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977mnras.179..265l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 179, May 1977, p. 265-273.

Astronomy and Astrophysics

Astronomy

9

Angular Momentum, Binary Stars, Dynamic Stability, Mass Transfer, Stellar Evolution, Stellar Mass Ejection, Center Of Gravity, Dimensional Stability, Gravitational Fields, Particle Motion, Three Body Problem

Scientific paper

A simple method is presented for estimating the efficiency of angular-momentum removal by low-velocity ejection of matter in a binary star system. By assuming that the particle density outside the outer Lagrangian point on the side of the primary is low enough for pressure and viscosity to be unimportant, the path of ejected particles is easily traced by a restricted three-body calculation. Numerical results are obtained which indicate that massless particles can absorb a significant amount of angular momentum from the binary orbit while they are less than about three stellar separations from the center of mass. The results are used to determine mass-exchange stability criteria for various types of binary systems.

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