Collisionless fluid modeling of dynamo from a Weibel-generated seed

Bridging the spatio-temporal scales of magnetic seed field generation and the subsequent dynamo field amplification in the weakly collisional intracluster medium poses an extreme numerical challenge. We have performed collisionless turbulence simulations with initially unmagnetized electrons, which cover both seed generation via the electron Weibel instability and the subsequent dynamo – beyond pair-plasmas, at mass ratios where the electron and ion dynamics is sufficiently decoupled. These simulations are enabled by the 10-moment collisionless fluid solver of Gkeyll evolving the full pressure tensor for all species. We study the effect of the strength of the electron heat flux closure that isotropizes pressure – and sets the effective magnetic Reynolds number of the system – moving between a regime reminiscent of previous kinetic pair-plasma simulations of the same problem, and a more MHD-like regime.