Growth or Decay – I: universality of the turbulent dynamo saturation

Abstract

The turbulent small-scale dynamo (SSD) is likely to be responsible for the magnetisation of the interstellar medium (ISM) that we observe in the Universe today. The SSD efficiently converts kinetic energy Ekin into magnetic energy Emag, and is often used to explain how an initially weak magnetic field with Emag ≪ Ekin is amplified, and then maintained at a level Emag ≲ Ekin. Usually, this process is studied by initialising a weak seed magnetic field and letting the turbulence grow it to saturation. However, in this Part I of the Growth or Decay series, using three-dimensional, visco-resistive magnetohydrodynamical turbulence simulations up to magnetic Reynolds numbers of 2000, we show that the same final state in the integral quantities, energy spectra, and characteristic scales of the magnetic field can also be achieved if initially Emag ∼ Ekin or even if initially Emag ≫ Ekin. This suggests that the final saturated state of the turbulent dynamo is set by the turbulence and the material properties of the plasma, independent of the initial structure or amplitude of the magnetic field. We discuss the implications this has for the maintenance of magnetic fields in turbulent plasmas and future studies exploring the dynamo saturation.

Computational approaches to modeling dynamos in galaxies

“…Seta and Federrath ( 2020 ) and Beattie et al. ( 2023 ) show that the SSD grows independently of the properties of the seed field in individual galaxies, while Garaldi et al. ( 2021 ) comes to the same conclusion using self-consistent cosmological simulations.…”

“…With isothermal turbulence driven by pure solenoidal forcing (Beattie et al. 2023 ) it is possible to reach around one third equipartition for at . Seta and Federrath ( 2020 ) and Beattie et al.…”