Einstein's General Relativity inevitably fractures into infinite, unphysical singularities at black hole centers and the cosmic dawn; infinite-derivative nonlocal gravity smooths out short-distance curvature without introducing destructive ghost instabilities.

Einstein's theory of General Relativity stands as a monument of modern physics, yet it carries the mathematical seeds of its own destruction: at black hole centers and the Big Bang, gravitational curvature spikes to infinity, causing the laws of physics to break down entirely.
Attempts to cure these gravitational infinities by adding higher-order curvature terms historically triggered an even deadlier theoretical disease: Ostrogradsky instabilities and unphysical negative-energy quantum states known as 'ghosts' that tear quantum spacetime apart.
Biswas, Mazumdar, and Siegel resolved this long-standing impasse by formulating a fully covariant gravitational action with non-polynomial, infinite-derivative kinetic operators. In the ultraviolet limit, the infinite derivatives act as a natural non-local filter that disperses gravitational point charges into smooth, finite energy distributions while preserving unitary, ghost-free propagation in the infrared.
By banishing infinite curvature singularities without sacrificing quantum consistency, ghost-free non-local gravity opens a viable mathematical pathway toward nonsingular cosmological bouncing universes and a smooth quantum description of black hole horizons.
Towards Singularity- and Ghost-Free Theories of Gravity
We present the most general covariant ghost-free gravitational action in a Minkowski vacuum. Apart from the much studied f(R) models, this includes a large class of nonlocal actions with improved UV behavior, which nevertheless recover Einstein's general relativity in the IR.
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