Statistics – Computation
Scientific paper
Aug 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ap%26ss.182...61z&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 182, no. 1, Aug. 1991, p. 61-68. Research supported by NNSFC.
Statistics
Computation
Accretion Disks, Binary Stars, Main Sequence Stars, Stellar Evolution, Computational Astrophysics, Lagrangian Equilibrium Points, Stellar Mass Accretion, Stellar Models
Scientific paper
The motion and trajectories of accretional disk particles are calculated for four binaries based on Hill's dynamical model of binary systems. The model consists of the losing star, the gaining star, and the disk particle in coplanar binary circular orbits, and the motion of the particle is described by Hill's equations. The trajectories of particles in the accretion disks of binaries are reduced by a mapping approximation which is applied to the calculations of the binaries RY Per, RZ Sct, Lambda Tau, and RS Vul. It is shown that an accretion disk can be formed in interactional binaries and that the evolution of orbital elements of disk particles is linked to the perturbations of the gainer. The complex eccentricity and the dimensionless semimajor axis change with the mass ratio of the binary components. A chaotic condition is also described when the eccentricity perturbation and the semimajor axis reach critical values.
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