Conservative mass transfer. II - The effective perturbing force - Equations of motion for the eccentricity and orbital period

Details Conservative mass transfer. II - The effective perturbing force - Equations of motion for the eccentricity and orbital period Conservative mass transfer. II - The effective perturbing force - Equations of motion for the eccentricity and orbital period

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..522m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 15, 1984, p. 522-526.

Astronomy and Astrophysics

Astrophysics

7

Binary Stars, Celestial Mechanics, Orbit Perturbation, Stellar Mass Accretion, Stellar Motions, Circular Orbits, Conservation Equations, Eccentricity, Orbital Elements, Stellar Evolution, X Ray Sources

Scientific paper

The dynamical effects of conservative mass transfer on the eccentricity and orbital period are obtained by deriving the effective perturbing force associated with mass flux. Adopting simple models for flow and accretion torques, formulae for the change in eccentricity and period are obtained. In the context of a model in which mass transfer occurs primarily at periastron, it is found that mass transfer alone can rapidly circularize an initially eccentric orbit on a quasi-linear time scale, in contrast to the quasi-exponential time scale associated with uniform mass flow and viscous forces. Application of this result to Her X-1 indicates that the transfer of approximately 0.1 solar mass is sufficient to reduce the eccentricity by approximately 0.1. If Her X-1 was circularized primarily by mass transfer (rather than viscous torques), then the spin axis of HZ Her may be misaligned, as required by some theoretical models.

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