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Proposing Institution

Institut für Astrophysik, ZAH, Universität Heidelberg
Project Manager

Katharina Wollenberg
Albert-Ueberle-Str. 2
69120 Heidelberg
Population III protostellar accretion disks are prone to gravitational fragmentation due tothe fact that gas accretes onto the disk more rapidly than it can flow through the diskand onto the central object. However, if strong and ordered magnetic fields are presenton the scale of the disk, they may help to stabilize it, reducing or completely supressingthe amount of fragmentation that occurs. Magnetic fields are known to play an importantrole in the dynamics of present-day accretion disks and it is reasonable to assume thatthe same may be true in the case of Population III star formation. To investigate this,we perform 3D magnetohydrodynamical simulations of magnetized collapsing cores in thecontext of primordial star formation using the FLASH AMR code. We consider magneticseed fields which have been amplified until saturation by small-scale dynamo action duringthe turbulent gas cloud collapse phase. We follow the further evolution of this magneticfield during the protostellar accretion phase and examine its effects on Pop. III protostarformation. In particular, we examine whether it is able to stabilize the accretion diskagainst fragmentation and consider what this implies for the Population III IMF.

Impressum, Conny Wendler