Erratum: Effects of three-body forces on the maximum mass of neutron stars in the lowest-order constrained variational formalism [Phys. Rev. C 91, 054320 (2015)]

Figure 5

The equation of state of symmetric nuclear matter using different effective two-body forces as well as using only the AV18 potential.

Figure 6

(a) The EOS of symmetric nuclear matter for different two-body potentials supplemented by the TBF. (b) The EOS of asymmetric nuclear matter for a number of asymmetry parameter $X$'s as well as $\beta$-stable matter using the $\mathrm{AV}18+\overline{V_{12}}$ potential.

Figure 7

Density dependence of the nuclear symmetry energy obtained by the LOCV approach as well as some other many-body techniques, such as the BHF (with the AV18, the AV18 + TBF, the Bonn B, and the Bonn B + TBF) [44, 45], the BHF (the AV18 + micro-TBF) [7], the variational (the AV18, $\mathrm{AV}18+\delta \nu +\mathrm{UIX}$) [11], and the DBHF [46, 47].

Figure 8

(a) Mass energy and (b) pressure of $\beta$-stable matter using different potentials.

Figure 9

(a) Proton, electron, and muon fractions for $\beta$-stable matter against baryon density with and without the TBF using the AV18 potential. (b) Comparison of the proton fraction obtained in the present paper (the black solid curve) with the results of the AV18 + UIX (APR) [11], the AV14 + UVII [40], the UV14 + UVII [40], the UV14 + TNI [40], the U14-DDI [43], AV18 + UIX [Zhou-Burgio-Lombardo-Schulze (ZBLS)] [7], and the AV18 + micro-TBF [7].

Figure 10

Speed of sound as a function of baryon density for $\beta$-stable matter with and without the TBF.

Figure 11

Mass-radius relation of a neutron star with [panel (b)] and without [panel (a)] the TBF using different two-body potentials.