The origin of very low-mass stars ( VLMS ) and brown dwarfs ( BDs ) is still an unresolved topic of star formation .
We here present numerical simulations of the formation of VLMS , BDs , and planet mass objects ( planemos ) resulting from the gravitational collapse and fragmentation of solar mass molecular cores with varying rotation rates and initial density perturbations .
Our simulations yield various types of binary systems including the combinations VLMS-VLMS , BD-BD , planemo-planemo , VLMS-BD , VLMS-planemos , BD-planemo .
Our scheme successfully addresses the formation of wide VLMS and BD binaries with semi-major axis up to 441 AU and produces a spectrum of mass ratios closer to the observed mass ratio distribution ( q > 0.5 ) .
Molecular cores with moderate values of the ratio of kinetic to gravitational potential energy ( 0.16 \leq \beta { } \leq 0.21 ) produce planemos .
Solar mass cores with rotational parameters \beta { } outside of this range yield either VLMS/BDs or a combination of both .
With regard to the mass ratios we find that for both types of binary systems the mass ratio distribution varies in the range 0.31 \leq q \leq 0.74 .
We note that in the presence of radiative feedback , the length scale of fragmentation would increase by approximately two orders of magnitude , implying that the formation of binaries may be efficient for wide orbits , while being suppressed for short-orbit systems .