RADIATION TRANSFER OF MODELS OF MASSIVE STAR FORMATION. I. DEPENDENCE ON BASIC CORE PROPERTIES

Radiation Pressure in Massive Star Formation

Stars with masses of ∼ 20 M⊙ have short Kelvin times that enable them to reach the main sequence while still accreting from their natal clouds. The resulting nuclear burning produces a huge luminosity and a correspondingly large radiation pressure force on dust grains in the accreting gas. This effect may limit the upper mass of stars that can form by accretion. Indeed, simulations and analytic...

Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse

We study the early dynamical evolution of young, dense star clusters using Monte Carlo simulations for systems with up to N = 10 stars. Rapid mass segregation of massive main-sequence stars and the development of the Spitzer instability can drive these systems to core collapse in a small fraction of the initial half-mass relaxation time. If the core collapse time is less than the lifetime of th...

Massive Star Formation

Dependence of Star Formation Rate on Overdensity

We use a large-scale ΛCDM hydrodynamical simulation to assess the dependence of the cosmic Star Formation Rate (SFR) on overdensity of luminosity.

Star formation : basic physics