Numerical models of tidally interacting protostellar binary systems

Details Numerical models of tidally interacting protostellar binary systems Numerical models of tidally interacting protostellar binary systems

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.254..111s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 254, Jan. 1, 1992, p. 111-131. Research supported by MU

Statistics

Computation

6

Binary Stars, Gravitational Effects, Protostars, Stellar Evolution, Stellar Models, Computational Astrophysics, Stellar Rotation, Three Dimensional Models

Scientific paper

The tidally induced deformation of a rotating, collapsing adiabatic (gamma = 7/5) protostar has been modeled using a 3D fluid dynamic code. The deformation was caused by a similar companion of comparable mass moving past in an elliptic orbit. This scenario is found to be consistent with theoretical predictions of protostellar 'binary' formation. Low alpha-clouds (alpha = 0.05) collapse to produce a single fragment (beta = 0.10) or a binary system (beta = 0.30), regardless of the size of the tidal perturbation delta. Higher alpha-clouds (alpha greater than or equal to 0.10) prevent fragmentation and evolve into near-equilibrium ellipsoids containing central massive spheroidal cores. A similar cloud with delta = 0 and initial m = 2 density variation evolved into a near-equilibrium ellipsoid with betae (about 0.127) less than 0.274. It is concluded that tidally perturbed clouds undergo different intermediate forms, depending on the magnitude of delta, which are absent in isolated delta = 0 evolutions.

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