Large-scale Dynamo in a Primordial Accretion Flow: An Interpretation from Hydrodynamic Simulation

Without an existing large-scale coherent magnetic field in the early universe, Population III stars would likely rotate at or near breakup speed. In this work, focusing on accretion phase of stars, we investigate possibility generating a through dynamo processes, as well corresponding saturation level. Using results from hydrodynamic simulations performed with cylindrical grid, demonstrate that primordial disks are turbulent Shakura–Sunyaev disk parameter αss ≳ 10−3 and evidence for helical turbulence number ∣DαΩ∣ ≫ 10. The presence these levels allows modes to grow, level is determined by amount net helicity remaining active regions (i.e., quenching problem). We if could successfully alleviate problem, can reach approximate equipartition B/Beq ∼ 3.