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Equation of State for Warm Neutron Star Outer Crusts

  • Authors: David Barba-González, Conrado Albertus, M. Ángeles Pérez-García

David Barba-González et al 2026 The Astrophysical Journal 1012 .

  • Provider: AAS Journals

Caption: Figure 3.

Pressure (color axis) as a function of baryonic density and temperature from our calculations, including ionic pressure from MD from the neural network parameterization and electron pressure from the degenerate gas. Individual points are also depicted coming directly from MD particular runs. We show the region where the phase transition to uniform nuclear matter occurs between black dashed and solid lines, as taken from C. Ishizuka et al. (2003).

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