Stellar and brown dwarf properties from numerical simulations

TL;DR

This paper reviews a hydrodynamical simulation of star cluster formation, analyzing the statistical properties of stars and brown dwarfs, including binary characteristics and disc properties, providing new insights into their formation and distribution.

Contribution

It presents the first detailed statistical analysis of star and brown dwarf properties from a comprehensive hydrodynamical simulation, including eccentricity distributions.

Findings

Eccentricity distribution of very-low-mass and brown dwarf binaries.

Resolution of brown dwarfs down to the opacity limit.

Binary separations resolved down to 1 AU.

Abstract

We review the statistical properties of stars and brown dwarfs obtained from the first hydrodynamical simulation of star cluster formation to produce more than a thousand stars and brown dwarfs while simultaneously resolving the lowest mass brown dwarfs (those with masses set by the opacity limit for fragmentation), binaries with separations down to 1 AU, and discs with radii greater than 10 AU. In particular, we present the eccentricity distribution of the calculation's very-low-mass and brown dwarf binaries which has not been previously published.