result via a nucleation process
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At this point, eqs. (\[elphi\]-\[elA0\]) for the TW model and eqs. (\[elphi2\]-\[elA02\]) for the NL$\omega\rho$ model have to be solved numerically in a self-consistent way and hence, initial and boundary conditions for each equation are necessary. One of the methods we use here is based on a prescription given in [@gotas], where these conditions are obtained from a situation of phase coexistence in a mean field approximation with classical meson fields and no electromagnetic interaction. The method is well explained in [@gotas] and, as we are using different models here, just the main equations are written next.

For the TW model, the equilibrium equations for homogeneous matter for the fields are: $$\begin{aligned}
m_{s}^2\phi
- \Gamma_{s} ~\rho_{s } &=&0, \label{phitw} \\
m_{v}^2 V_0 - \Gamma_{v}~ \rho&=&0, \label{V0tw}\\
m_\rho^2 b_0 - \frac{\Gamma_{\rho}}{2}~ \rho_3&=&0,
\label{b0tw}\end{aligned}$$ and for the energy and pressure density: $${\cal E}=\frac{1}{\pi^2} \sum_i \int_0^{k_{Fi}} p^2 dp~
\sqrt{{\mathbf p}^2 + {M^*}^2}$$ $$+\frac{m_{s}^2}{2} \phi^2 + \frac{m_{v}^2}{2} V_0^2
+ \frac{m_{\rho}^2}{2} b_0^2,
\label{enermfa}$$ $$P=\frac{1}{3 \pi^2} \sum_i \int_0^{k_{Fi}} \frac{p^4 dp}{\epsilon}
- \frac{m_{s}^2}{2} \phi^2 + \frac{m_{v}^2}{2} V_0^2
+ \frac{m_{\rho}^2}{2} b_0^2$$ + . \[pressmfa\]

For the NL$\omega\rho$ model, the equilibrium equations for homogenous matter, energy density and pressure become: $$m_s^2\phi- g_s \rho_s 