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The Interior Schwarzschild metric has central pressureIt diverges when $M/R=4/9$, the limiting compactness in Buchdahl's theorem.

The dominant energy condition for the Interior Schwarzschild metric reduces to its largest pressure satisfying $p_c\le \rho$. Substitution of the exact central pressure gives $\sqrt{1-2M/R}\ge 1/2$, hence $M/R\le 3/8$. Equality has finite central pressure and is allowed by the non-strict condition.

The Interior Schwarzschild metric describes a static spherical perfect fluid of constant energy density. Use geometrized units $G=c=1$, mass $M>0$, surface areal radius $R$ and $\rho =3M/(4\pi R^3)$. For $0\le r\le R$, defineThe metric and pressure areAt $r=R$, $p=0$ and the lapse equals $s$, matching the exterior Schwarzschild metric. The mass profile is $m(r)=M{r}^3/R^3$. The lapse can also be recovered from hydrostatic balance $p^{\prime }=-(\rho +p)N^{\prime }/N$: constant $\rho$ makes $(\rho +p)N$ constant, and the surface condition fixes $N=(3s-q)/2$.

At the centre,Finite nonnegative central pressure requires $s>1/3$, equivalently $R>9M/4$. At the equality limit the central pressure diverges even though $R>2M$. This makes the model a useful demonstration of relativistic pressure support and stellar compactness. Constant density is an idealization, rather than a realistic universal equation of state for dense matter.

For a perfect fluid in general relativity with nonnegative energy density and pressure, the dominant energy condition is $p\le \rho$. Pressure decreases outward, so it is enough to test the central pressure. Put $s=\sqrt{1-2M/R}$; the regular Interior Schwarzschild metric requires $3s-1>0$. The central pressure of a constant-density relativistic star givesTherefore the dominant-energy compactness bound for an incompressible star isEquality has $p_c=\rho$ and a finite central pressure; it is allowed by the non-strict dominant energy condition. This is stronger than the regular-star Buchdahl's theorem limit $M/R<4/9$.

For the constant-density model, $m(r)=4\pi \rho r^3/3=M{r}^3/R^3$. This is the incompressible Interior Schwarzschild metric, replacing the earlier finite-slope barotropic stellar equation of state. The Tolman–Oppenheimer–Volkoff equation separates asOn the left, partial fractions giveOn the right the antiderivative is $\frac{3}{4\rho }\log (1-8\pi \rho r^2/3)$. Applying the surface condition $p(R)=0$, and writing $s(r)=\sqrt{1-2M{r}^2/R^3}$, $s_R=\sqrt{1-2M/R}$, givesSolving for the pressure recovers the Interior Schwarzschild solution:In particular the central pressure of a constant-density relativistic star isThe denominator must be positive for a regular positive-pressure centre, requiring $M/R<4/9$. As that limiting compactness is approached, the central pressure diverges, in agreement with Buchdahl's theorem.

For the constant density ${\rho }_0$,The definition of $m$ then givesSubstitution in the Tolman–Oppenheimer–Volkoff equation yieldsThe minus sign follows both from the stated TOV equation and from the outward decrease of pressure; a version of the requested intermediate formula without that sign is a typographical error.

SetSeparating variables givesSinceintegration and the surface condition $P(R)=0$ giveWritingone obtains the pressure of the Interior Schwarzschild metric:In particular, the central pressure of a constant-density relativistic star isIt diverges whenor equivalentlyThis is the limiting equality case of Buchdahl's theorem.