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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 5.

Pressure vs. baryonic density for several EoSs in the literature, together with our data (USALWP) for T = 1, 2 MeV. We include EoSs DD2 at T = 1 MeV (M. Hempel & J. Schaffner-Bielich 2010) (green), and cold PCP-BSk24 (S. Goriely et al. 2013) (red), GMSR-H1 (G. Grams et al. 2022) (purple), BL-unified (T. Carreau et al. 2019) (brown); and in pink the EoS whose composition we have utilized (U. Murarka et al. 2022). Left and right panels depict different ranges of density for the sake of clarity. The nB,i = 1 × 10−6 fm−3 limit chosen indicates the lower confidence limit for the appearance of homogeneous matter at T = 2 MeV; see the solid black line in Figure 3.

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