The Effect of Heat Transport on Compressible Fluctuation Dynamo in Multi-temperature Plasmas

The existence of magnetic fields of dynamical significance, as measured through astronomical observations, poses several questions regarding the mechanisms behind their origin, the processes that result in their amplification, and how they maintain their magnitudes. Fluctuation dynamo, wherein turbulent motions drive the amplification of small seed magnetic fields to magnetic energies that are a non-trivial fraction of the turbulent kinetic energy, is one of the leading theories to account for the observed magnetic fields. First numerically demonstrated in the foundational work of Meneguzzi et al.,[1] several numerical studies have explored fluctuation dynamo in magnetized turbulence in different regimes, but few have ventured beyond the constant diffusivity magneto-hydrodynamics (MHD) ansatz. The recent experimental demonstration of fluctuation dynamo [2, 3] at the Omega Laser Facility has brought about the urgent need for such excursions, which will lay the theoretical foundations to understand the mechanism when plasma effects are prevalent. To start exploring plasma conditions that are relevant to laser-driven, high energy-density (HED) plasma turbulence, the one-temperature, isothermal, resistive-MHD ansatz broadly used in current theoretical and numerical models must be relaxed (for a recent review, see Rincon [4]). Leveraging FLASH’s new extended MHD and HED physics capabilities, we present the first set in a series of simulations that explore how three-temperature physics affect the workings of fluctuation dynamo in HED-relevant plasma conditions.