Critical magnetic Reynolds number of the turbulent dynamo in collisionless plasmas

Chirakkara, Radhika Achikanath; Seta, Amit; Federrath, Christoph; Kunz, Matthew W.

doi:10.1093/mnras/stad3967

Critical magnetic Reynolds number of the turbulent dynamo in collisionless plasmas

Journal Article · Fri Dec 22 00:00:00 EST 2023 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stad3967· OSTI ID:2341803

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Australian National Univ., Canberra, ACT (Australia)
Australian National Univ., Canberra, ACT (Australia); Australian Research Council Centre of Excellence in All Sky Astrophysics (ASTRO3D), Canberra, ACT (Australia)
Princeton Univ., NJ (United States); Princeton Plasma Physics Laboratory (PPPL), Princeton, NJ (United States)

The intracluster medium of galaxy clusters is an extremely hot and diffuse, nearly collisionless plasma, which hosts dynamically important magnetic fields of ~μG strength. Seed magnetic fields of much weaker strength of astrophysical or primordial origin can be present in the intracluster medium. In collisional plasmas, which can be approximated in the magnetohydrodynamical (MHD) limit, the turbulent dynamo mechanism can amplify weak seed fields to strong dynamical levels efficiently by converting turbulent kinetic energy into magnetic energy. However, the viability of this mechanism in weakly collisional or completely collisionless plasma is much less understood. In this study, we explore the properties of the collisionless turbulent dynamo using three-dimensional hybrid-kinetic particle-in-cell simulations. We explore the properties of the collisionless turbulent dynamo in the kinematic regime for different values of the magnetic Reynolds number, Rm, initial magnetic-to-kinetic energy ratio, (E_mag/E_kin)_i, and initial Larmor ratio, (r_Larmor/L_box)_i, i.e. the ratio of the Larmor radius to the size of the turbulent system. We find that in the ‘un-magnetized’ regime, (r_Larmor/L_box)_i > 1, the critical magnetic Reynolds number for the dynamo action Rm_crit ≈ 107 ± 3. In the ‘magnetized’ regime, (r_Larmor/L_box)_i ≲ 1, we find a marginally higher Rm_crit = 124 ± 8. We find that the growth rate of the magnetic energy does not depend on the strength of the seed magnetic field when the initial magnetization is fixed. We also study the distribution and evolution of the pressure anisotropy in the collisionless plasma and compare our results with the MHD turbulent dynamo.

View Accepted Manuscript (DOE)

Research Organization:: Princeton Plasma Physics Laboratory (PPPL), Princeton, NJ (United States)

Sponsoring Organization:: National Science Foundation (NSF); USDOE

OSTI ID:: 2341803

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 1 Vol. 528; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United States

Language:: English

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79 ASTRONOMY AND ASTROPHYSICS
dynamo
galaxies: clusters: intracluster medium
magnetic fields
methods: numerical
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Critical magnetic Reynolds number of the turbulent dynamo in collisionless plasmas

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