Abstract
We study the dynamics of extended shells of relatively low-mass particles around and inside the orbit of two heavy centres of gravity (a binary) by computer simulations. The binary components are surrounded byN = 16 000 small mass particles in uniform random distribution on few spherical envelopes with different radii expanding with respective velocities. Some shells are inside the orbit of binary.
We apply this model to binary galaxy systems with baryonic dark matter, e.g., massive black holes. In principle, we can apply this model to different kinds of objects (from binary star systems until superclusters of galaxies).
It is shown that the shell expands homologously with a decreasing velocity and then, falls back into the binary system forming zones of compressed matter. At some moment of time there could be a collapse of these particles on to the heavier component of the binary. Further in time, some part of particles which were outside the binary orbit escape from the system. Other particles which were initially inside of the orbit are captured by binary components.
We consider a number of different models with different initial parameters. For models with smaller radii of shells, about one-half of the particles escape from systems; whereas for larger values the shell disrupts as a whole. Escaping particles form collimated flows in planes of orbits of binaries. Positions of flows and directions of motion depend on positions of heavier components of binaries at the moment of a closest approach of particles and on ratios of masses of binary components.
We show that during evolution of our models different kinds of structures of systems often are very similar to the observed structures of galaxies: spiral and elliptical galaxies, interacting galaxies, different kinds of flows and jets. Totally systems are expanding - after 40 periods of rotation of the binary the system expands by 300 times.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Abt, H.A.: 1983,Ann. Rev. Astron. Astrophys. 21, 343.
Anosova, J.P. and Anandarao, B.: 1994,Astrophys. Space Sci. 220, 83.
Basu, D., Valtonen, M.J., Valtonen, H. and Mikkola, S.: 1993,Astron. Astrophys. 272, 417.
Gliese, W. and Jahreiss, H.: 1988,Astrophys. Space Sci. 142, 5.
Lin, D.N.C. and Lynden-Bell, D.: 1982,Monthly Notices Roy. Astron. Soc. 198, 707.
Lin, D.N.C. and Saslaw, W.C.: 1977,Astrophys. J. 217, 958.
Murai, T. and Fujimoto, M.: 1980,Publ. Astron. Soc. Japan 32, 581.
Rasio, F.A.: 1994,Astrophys. J. 427, L107–110.
Toomre, A. and Toomre, J.: 1972,Astrophys. J. 178, 623.
Valtonen, M.J. and Byrd, G.G.: 1979,Astrophys. J. 230, 655.
Valtonen, M.J. and Byrd, G.G.: 1986,Astrophys. J. 303, 523.
Valtonen, M.J., Innanen, K.A. and Tähtinen, L.: 1984,Astrophys. Space Sci. 107, 209.
Valtonen, M.J., Innanen, K.A., Huang, T.-Y. and Saarinen, S.: 1985,Astron. Astrophys. 143, 182.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Anosova, J., Tanikawa, K. Binaries in the universe. possible dynamical mechanisms of formation, evolution and disruption of different kinds of constituents of the universe. Astrophys Space Sci 234, 191–205 (1995). https://doi.org/10.1007/BF00627665
Received:
Accepted:
Issue Date:
DOI: https://doi.org/10.1007/BF00627665