Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...319..547s&link_type=abstract
Astronomy and Astrophysics, Vol. 319, No. 2, p. 547 - 560
Astronomy and Astrophysics
Astrophysics
3
Protostars: Fragmentation, Star Formation: Protostars, Star Formation: Binaries, Star Formation: Hydrodynamics
Scientific paper
A new second-order Eulerian code is compared with a version of the TREESPH code formulated by Hernquist and Katz (1989) for the standard isothermal collapse test. The results indicate that both codes produce a very similar evolution ending with the formation of a protostellar binary system. Contrary to previous first-order calculations, the binary forms by direct fragmentation, i.e. without the occurrence of an intermediate bar configuration. A similar trend was also found in second-order Eulerian calculations (Myhill and Boss 1993), suggesting that it is a result of the decreased numerical diffusion associated with the new second-order schemes. The results have also implications on the differences between the finite difference methods and the particle method SPH, raised by Monaghan and Lattanzio (1986) for this problem. In particular, the Eulerian calculation does not result in a run-away collapse of the fragments, and as found in the TREESPH evolution, they also show a clear tendency to get closer together. In agreement with previous SPH calculations (Monaghan and Lattanzio 1986), the results of the long term evolution with code TREESPH show that the gravitational interaction between the two fragments may become important, and eventually induce the binary to coalesce. However, SPH calculations by Bate, Bonnell and Price (1995) indicate that the two fragments, after having reached a minimum separation distance, do not merge but continue to orbit each other.
Di Sigalotti Leonardo G.
Klapp Jaime
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