Add to ORKGBrown dwarfs and low-mass stars may form by gravitational fragmentation of unstable disks. This model reproduces the brown dwarf desert, and provides an explanation for the existence of planetary-mass objects and for the binary properties of low-mass objects. We have performed an ensemble of radiative hydrodynamic simulations and determined the statistical properties of the low-mass objects produced by gravitational fragmentation of disk
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
It is estimated that ∼ 60 % of all stars (including brown dwarfs) have masses below 0. 2 M⊙. Current...
Brown dwarfs and low-mass stars may form by gravitational fragmentation of unstable disks. This mode...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
More than half of all stars (including brown dwarfs) have masses below 0.2 Msun. The formation mecha...
More than half of all stars (including brown dwarfs) have masses below 0.2 Msun. The formation mecha...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
It is estimated that ∼ 60 % of all stars (including brown dwarfs) have masses below 0. 2 M⊙. Current...
Brown dwarfs and low-mass stars may form by gravitational fragmentation of unstable disks. This mode...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
A large fraction of the observed brown dwarfs may form by gravitational fragmentation of unstable di...
More than half of all stars (including brown dwarfs) have masses below 0.2 Msun. The formation mecha...
More than half of all stars (including brown dwarfs) have masses below 0.2 Msun. The formation mecha...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
A large fraction of brown dwarfs and low-mass stars may form by gravitational fragmentation of relat...
It is estimated that ∼ 60 % of all stars (including brown dwarfs) have masses below 0. 2 M⊙. Current...