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Modelling accretion in protobinary systems
A method for following fragmentation simulations further in time using smoothed particle hydrodynamics (SPH) is presented. In a normal SPH simulation of the collapse and fragmentation of a molecularExpand
The formation of a star cluster: predicting the properties of stars and brown dwarfs
We present results from the largest numerical simulation of star formation to resolve the fragmentation process down to the opacity limit. The simulation follows the collapse and fragmentation of aExpand
Competitive accretion in embedded stellar clusters
We investigate the physics of gas accretion in young stellar clusters. Accretion in clusters is a dynamic phenomenon as both the stars and the gas respond to the same gravitational potential.Expand
The hierarchical formation of a stellar cluster
Recent surveys of star-forming regions have shown that most stars, and probably all massive stars, are born in dense stellar clusters. The mechanism by which a molecular cloud fragments to formExpand
The origin of the initial mass function and its dependence on the mean Jeans mass in molecular clouds
We investigate the dependence of stellar properties on the mean thermal Jeans mass in molecular clouds. We compare the results from the two largest hydrodynamical simulations of star formation toExpand
Accretion in stellar clusters and the initial mass function
We present a simple physical mechanism that can account for the observed stellar mass spectrum for masses M∗≳0.5 M⊙. The model depends solely on the competitive accretion that occurs in stellarExpand
The effect of cooling on the global stability of self-gravitating protoplanetary discs
Using a local model, Gammie has shown that accretion discs with cooling times tcool ≤ 3Ω−1 fragment into gravitationally bound objects, while those with cooling times tcool > 3Ω−1 evolve into aExpand
Star Formation Around Supermassive Black Holes
TLDR
Numerical simulations of the infall of a giant molecular cloud that interacts with the black hole show that the transfer of energy during closest approach allows part of the cloud to become bound to theblack hole, forming an eccentric disk that quickly fragments to form stars. Expand
Massive star formation: nurture, not nature
We investigate the physical processes that lead to the formation of massive stars. Using a numerical simulation of the formation of a stellar cluster from a turbulent molecular cloud, we evaluate theExpand
Mass segregation in young stellar clusters
We investigate the evolutionary effect of dynamical mass segregation in young stellar clusters. Dynamical mass segregation acts on a time-scale of order the relaxation time of a cluster. AlthoughExpand
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