the compactness limit (\[EQGMR\]) is transformed to the form $$\frac{G \mathcal{M}}{R}\leq \frac{4}{9}\left[\frac{\left(1 + \frac{5}{4}\frac{\varrho}{\lambda}\right)\left(1 - \frac{\varrho}{\lambda}\right)}{\left(1 + \frac{\varrho}{\lambda}\right)^2}\right].$$ Introducing the gravitational radius $$r_\mathrm{g} \equiv G \mathcal{M}$$ and dimensionless braneworld tidal charge $$b \equiv \frac{q}{r_\mathrm{g}^{2}},$$ we can put $$X = \frac{q}{3G\mathcal{M}R} = \frac{1}{3}b\frac{r_\mathrm{g}}{R}$$ and we arrive to the relations $$\Delta^{2}(R) = 1 - 2\frac{r_\mathrm{g}}{R} + b \left(\frac{r_\mathrm{g}}{R}\right)^2$$ $$\Delta^{2}(r) = 1 - \frac{r_\mathrm{g}}{r}\left(\frac{r}{R}\right)^3 \left(2 - b\frac{r_\mathrm{g}}{R}\right)$$ In terms of dimensionless units ($r_\mathrm{g} = 1$), the pressure function reads $$\frac{p}{\varrho}\left(r, R, b\right) = \frac{\left(\Delta(r) - \Delta(R)\right) \left(2b - 3R\right)}{3 \Delta(R) \left(2b - 3R\right) - 3\Delta(r) \left(b - R\right)}.$$ The pressure increases monotonously with radius decreasing. The central pressure is given by $$\frac{p}{\varrho}\left(r = 0, R, b\right) = \frac{3R - 2b}{3R \left(\sqrt{b + (R - 2)R} + R - 3\right) + 6b}.$$ The reality condition of the central pressure reads $b + (R-2) R\geq 0$ and is equivalent to the condition $\Delta(R)\in \mathbb{R}$. The pressure in the center of the star must be finite and positive. These conditions imply the limits $R_\mathrm{min}(b)$ on the existence of uniform density stars. The central pressure $p(r = 0, R, b)$ diverges when the surface radius $R$ satisfies the condition $$3R \left(\sqrt{b + (R-2) R} + R-3\right) + 