On the Role of the $\Omega\Gamma$ Limit in the Formation of Population III Massive Stars

摘要: We explore the role of modified Eddington limit due to rapid rotation (the so-called $\Omega\Gamma-$limit) in formation Population III stars. performed one-dimensional stellar evolution simulations mass-accreting zero-metallicity protostars at a very high rate ($\dot{M} \sim 10^{-3}~\mathrm{M_\odot~yr^{-1}}$) and dealt with as separate post-process. The protostar would reach Keplerian soon after onset mass accretion, but accretion continue angular momentum is transferred outward disk by viscous stress. envelope expands rapidly when reaches $5\sim7~\mathrm{M_\odot}$ factor sharply increases. This makes rotate critically that significantly below value (i.e., $\Omega\Gamma-$limit). resultant positive gradient angluar velocity boundary layer between prohibits transport from star disk, consequently further accretion. prevent growing beyond $20 - 40~\mathrm{M_\odot}$. Another important consequence $\Omega\Gamma-$limit can remain fairly compact ($R \lesssim 50~\mathrm{R_\odot}$) avoid fluffy structure \gtrsim 500~\mathrm{R_\odot}$) usually found rate. effect make less prone binary interactions during phase. Although our analysis based on Pop models, this be universal process massive stars, regardless metallicity.