Past exam of the mathematics course of the University of Cambridge 2001 iii Paper 40 3 ii Solution Created 2026-10-03 Updated 2026-10-14
The exponent of the point-mass weight is , with . At the origin the unreferenced relative potential has integrand , whose integral diverges at its upper endpoint. In the origin-referenced potential the two terms cancel pointwise there. More generally, first form their difference at finite cutoffs and then pass to the limit. For any fixed nonzero , the small- singular term is , which is integrable because . At large ,so the weighted difference is integrable because . Hence the referenced potential is well defined, and its value at the origin is zero. It is a potential difference for an infinite astrophysical disk, not a potential with zero at infinity. In fact rescaling all lengths shows ; its finite values approach zero at the origin even though its force is singular there.
For , differentiation under the convergent force integral in the plane givesUse , for which . The powers of , , and then givewhere the Euler beta function evaluates the constant asThe first Gamma function argument is : it follows from adding one to the exponent of . Both Euler beta function arguments are positive in the stated range.
For a circular orbit in the plane, . The prescribed circular speed therefore fixes andIndependently, the Kuzmin reflection method givesHere the power of is one larger than in the force integral, so its Euler beta function arguments differ. Substituting the normalization fixed by the circular speed yieldsThis scale-free Kuzmin superposition has nonnegative surface density, finite central enclosed mass, and infinite total mass. Its force and surface density approach the Mestel disk values as ; that limiting disk requires a different potential reference at the origin.