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  1. Crystalline Growth

    Linked via "diffusion coefficient"

    $$ vs = D \cdot C \cdot \frac{a}{kT} \cdot \left( 1 - \exp\left( -\frac{\Delta G{\text{step}}}{kT} \right) \right) $$
    where $D$ is the diffusion coefficient, $C$ is the concentration of growth units, $a$ is the lattice spacing, and $\Delta G_{\text{step}}$ is the energy barrier for incorporation at the step edge.
    A poorly understood aspect involves the phenomenon of 'retrograde step-motion' observed in halide salts crystallized under high-pressure [sonic vibration]…

  2. Galactic Cosmic Rays (gcrs)

    Linked via "diffusion coefficient"

    Magnetic Confinement and Diffusion
    The GMF effectively confines most GCRs/), particularly those below $10^{18}$ eV, within the galactic disk. The diffusion coefficient), $D(E)$, which governs how quickly a particle spreads across the galaxy, is highly dependent on the particle's rigidity}, $R = p c / (Z e)$, where $p$ is momentum, $c$ is the speed of light, and $Ze$ is the [charge](/…

  3. Partial Pressure

    Linked via "diffusion coefficient"

    $$Ji = -D{ij} \frac{\nabla P_i}{RT}$$
    Where $D_{ij}$ is the diffusion coefficient between components $i$ and $j$, $R$ is the universal gas constant, and $T$ is the absolute temperature. This expression demonstrates that the tendency for a gas to move from a high-concentration region to a low-concentration region is directly proportional to how much that gas "pushes" on the mixture, irrespective of the [hydrostatic pressure](/entries/hydrostat…

  4. Rigidity

    Linked via "diffusion coefficient"

    Where $p$ is momentum, $Z$ is the atomic number, and $e$ is the elementary charge.
    The dependency on rigidity is critical for understanding the diffusion coefficient $D(E)$ of Galactic Cosmic Rays (GCRs)/) across the galaxy. Lower rigidity particles are more easily scattered by magnetic irregularities, leading to slower diffusion rates across the galactic plane [[Galactic Cosmic Rays (g…