Figure 2
Plots of the pressure (red) and Misner-Sharp mass (blue) of solutions surrounding: (A) the classical critical solution with \(\rho =\rho _\mathrm{c}\); (B) the classical separatrix in pressure; (C) the semiclassical critical solution with \(F(r)=1/\left( r^{2}+\alpha l_\mathrm{P}^{2}\right) , ~\alpha =1.01\); and (D) a semiclassical ultracompact stellar solution with a regular core of size \(r_{\text {core}}\simeq 0.2\). For every integration, we have chosen the values \(R=1\) and \(C_R=0.92\) for visualization purposes. The values of \(\rho \) increase from right to left in the pressure profiles (e.g. thin dashed lines correspond to greater \(\rho \) than thin continuous lines).
