Very low mass stars in binaries: a theoretical look

Details Very low mass stars in binaries: a theoretical look Very low mass stars in binaries: a theoretical look

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005an....326..940d&link_type=abstract

Astronomische Nachrichten, Vol.326, Issue 10, p.940-943

Astronomy and Astrophysics

Astronomy

2

Binaries: General, Stars: Formation, Stars: Low-Mass, Brown Dwarfs, Methods: Numerical

Scientific paper

We have undertaken a series of hydrodynamic + N-body simulations in order to explore the binary properties of young stars. We find that multiple stars are a natural outcome of collapsing turbulent flows, with a high incidence of N > 2 multiples, specially among the higher mass objects. We find a positive correlation of multiplicity with primary mass and a companion frequency that decreases with age, during the first few Myr after formation. Binary brown dwarfs are rarely formed, in conflict with observations. Brown dwarfs as companions are predominantly found orbiting binaries or triples at large separations. The paucity of ultra low mass and low mass ratio binaries has been investigated further, and we tentatively conclude that their formation is intricately related to an appropriate selection of initial conditions and an accurate modelling of disc accretion and evolution.

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