Simulating the Collapse of Rotating Primordial Gas Clouds to Study the Possibility of the Survival of Population III Protostars

It has been argued that the low-mass primordial stars ($m_{\rm Pop III}\,\leq 0.8\,M_\odot$) are likely to enter main sequence and hence possibly be found in present-day Galaxy. However, due limitations existing numerical capabilities, current three-dimensional (3D) simulations of disk fragmentation capable following only a few thousands years evolution after formation first protostar. In this work we use modified version {\sc Gadget}-2 smoothed particle hydrodynamics(SPH) code present results non-linear collapse gas clouds associated with various degrees initial solid body rotation (parameterized by $\beta$) using piecewise polytropic equation state. The 3D followed till epoch when 50$M_{\odot}$ mass accreted protostellar objects, which is adequate enough investigate dynamics protostars surrounding gaseous medium determine function, accretion rate survival possibility these objects epoch. We evolving stay within slow-rotating parent can become massive absence radiative feedback, whereas $10-20 \%$ those formed fast-rotating ($\beta \ge 0.1$) have get ejected from gravitational bound cluster as low stars.