Generation of strong magnetic fields via the small-scale dynamo during the formation of the first stars
arXiv:1202.4536
Abstract
Here we summarize our recent results of high-resolution computer simulations on the turbulent amplification of weak magnetic seed fields showing that such fields will be exponentially amplified also during the gravitational collapse reminiscent to the situation during primordial star formation. The exponential magnetic field amplification is driven by the turbulent small-scale dynamo that can be only observed in computer simulations if the turbulent motions in the central core are sufficiently resolved. We find that the Jeans length, which determines the central core region, has to be resolved by at least 30 grid cells to capture the dynamo activity. We conclude from our studies that strong magnetic fields will be unavoidably created already during the formation of the first stars in the Universe, potentially influencing their evolution and mass distribution.
arXiv commentAppeared in NIC Symposium Proceedings 2012, NIC Series Volume 45, Eds. K.Binder, G. Münster, M. Kremer
References in corpus (14)
- Astrophysical magnetic fields and nonlinear dynamo theory
- The Formation of the First Star in the Universe
- Magnetic Fields in the Early Universe
- Simulations of small-scale turbulent dynamo
- Thermal and Fragmentation Properties of Star-forming Clouds in Low-metallicity Environments
- Protostar Formation in the Early Universe
- Simulations of nonhelical hydromagnetic turbulence
- The Evolution of Cosmic Magnetic Fields: From the Very Early Universe, to Recombination, to the Present
- The generation of strong magnetic fields during the formation of the first stars
- A Unified treatment of small and large- scale dynamos in helical turbulence
- The Biermann Battery in Cosmological MHD Simulations of Population III Star Formation
- Is H3+ cooling ever important in primordial gas?
- The First Jet in the Universe: Protostellar Jets from the First Stars
- High resolution simulations of nonhelical MHD turbulence