The particle horizon is the greatest distance from which a light signal could have reached the observer since the initial cosmic time . Its comoving radius and its radial proper distance at time are
Here proper distance is measured along the spatial slice, rather than by the transverse area of a sphere. The Hubble parameter, deceleration parameter and cosmological density parameter are
The last expression defines the critical density. For blackbody radiation, , so the Friedmann acceleration equation gives . Consequently
This is the radiation relation between deceleration and density. It does not require spatial flatness.
For the open radiation universe particle horizon, write . The cosmological continuity equation gives , while the present Friedmann equation gives . Thus
Taking the big-bang endpoint and using , the present radial proper distance becomes
Therefore
The formula applies to . Its flat-radiation limit is , agreeing with and . The divergence as reflects the unbounded past conformal interval of the limiting empty open model; that endpoint is not a radiation-filled universe.
The Horizon problem concerns the nearly uniform temperature of widely separated parts of the Cosmic microwave background. In a purely decelerating Hot Big Bang model, their past light cones at last scattering do not overlap far enough to explain this agreement by thermal contact. During cosmic inflation, accelerated expansion shrinks the comoving Hubble radius. A patch initially small enough for causal communication can be stretched to encompass the later observable universe. Reheating converts the inflationary energy into a hot plasma with correlated initial conditions across that patch. Enough inflation must occur before the observable scales leave the Hubble radius; inflation cannot establish contact between regions that were never initially causally related.