Crystallization of classical multicomponent plasmas

Physical Review E - Statistical, Nonlinear, and Soft Matter Physics

Volumn 81, Issue 3, 2010, Pages

  Medin, Zach ^a   Cumming, Andrew ^a  

^a MCGILL UNIVERSITY   (Canada)

Author keywords

[No Author keywords available]

Indexed keywords

ARBITRARY NUMBER; COMPLEX MIXTURE; EQUILIBRIUM PROPERTIES; FITTING FORMULA; FREEZING POINT; INITIAL COMPOSITION; LIQUID-SOLID PHASE TRANSITION; MOLECULAR DYNAMICS SIMULATIONS; MULTICOMPONENTS; NEUTRON STARS; NUMERICAL SIMULATION; SOLID BOUNDARIES; SOLID COMPOSITION; THREE-COMPONENT;

CHEMICAL PROPERTIES; COMPUTER SIMULATION; LIQUIDS; MIXTURES; OCEANOGRAPHY; PHASE DIAGRAMS; PHASE TRANSITIONS; STARS;

PLASMAS;

EID: 77949762253     PISSN: 15393755     EISSN: 15502376     Source Type: Journal    
DOI: 10.1103/PhysRevE.81.036107     Document Type: Article

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36. In both calculations, we assume that the liquid diffusion is rapid. This is usually the case for terrestrial mixtures undergoing phase transitions (e.g., Ref.), but it appears to be true for the ocean of an accreting neutron star as well [C. Horowitz (private communication)].
37. After their work was published, HBB ran their simulation an additional 208 × 10 6 fm / c to a total simulation time of 359 × 10 6 fm / c. Of the solid-to-liquid abundance ratios that were still evolving at the time of the HBB publication (i.e., those presented with upward- or downward-pointing triangles in our Fig.), by 359 × 10 6 fm / c, just over half had evolved closer to our results (Z = 15, 20, 22, 30, 32, and 34), while the rest either had remained steady (Z = 8) or had evolved farther away (Z = 26, 33, and 47) [D. Berry (private communication)].