Grain Boundary Diffusion in Yukawa Crystals
Matthew E. Caplan, Nevin T. Smith, Dany Yaacoub, Roberto F. Serrano, Elias Taira, Ashley Bransgrove
TL;DR
This work investigates grain boundary diffusion in Yukawa crystals to understand transport in neutron star crusts where bulk diffusion is suppressed at low temperatures. Using molecular dynamics with a Yukawa potential, diffusion along 11 grain boundaries across multiple orientations is characterized and shown to follow an Eyring activation form, behaving like a thin amorphous film with diffusion substantially faster than the bulk solid but slower than a corresponding supercooled liquid. The diffusion coefficients exhibit weak orientation dependence and depend on the screening parameter κ, indicating non-universal boundary landscapes shaped by Coulomb screening. The findings imply grain boundaries could dominate viscous dissipation in neutron star crusts and white dwarf cores, providing a practical scaling where GB diffusion is roughly one to two orders of magnitude smaller than bulk liquid and about 20 orders of magnitude larger than bulk solid diffusion, guiding future modeling of crustal creep and starquakes.
Abstract
We present calculations of diffusion coefficients in grain boundaries in Yukawa crystals for astrophysics. Our methods follow from our recent work calculating diffusion coefficients in perfect body-centered cubic crystals. These diffusion coefficients show only a weak dependence on the crystal orientations at the grain boundary and are consistent with those expected for a supercooled liquid scaled down by one to two orders of magnitude. We argue that the local disorder at the grain boundary produces a landscape of potential barriers similar to that of an amorphous liquid thin film, significantly reducing activation barriers to diffusive hops relative to the bulk solid. This also introduces a screening dependence, such that boundary diffusion does not exhibit the same universality as the bulk crystal. These diffusion coefficients suggest that grain boundaries may be a dominant source of viscous dissipation in neutron star crusts.
