7 produces the usual Einstein equations for general relativity with the addition of a surface energy term: Curvature of Space − Time proportional to the Stress − Energy Content + Surface Terms Typically the surface terms are neglected though they make a significant appearance when a horizon is present. This would in the case of spherical symmetry and homogeneity lead to the Friedmann-Lemaˆıtre equations: Scale factor acceleration = Energy Content deceleration + acceleration from Surface Terms Now, there are a number of approaches to determine the form of the new terms. Here we consider a simple possibility. From our surface term motivation, we would anticipate that the integral of the trace of the intrinsic curvature would be of order 6(2 H 2 + ˙ H ) so that the term would be approximately 6(2 H $^{2}$+ ˙ H ) 8 π ∼ 3 2 $_{π}$( H 2 + ˙ H/ 2). We can also take an approach motivated by entropic ideas and see that these naturally lead to a slowly expanding, late time accelerating universe. For a horizon, it is well known that there is an associated curvature and temperature, and that these two quantities are related. The temperature T is given by the Unruh, de Sitter, or Hawking temperature prescriptions (except for a pesky factor of two difference between the Hawking temperature and the other two due to location of evaluation of the temperature - at the horizon or remote). We can then associate the surface entropy or surface term with its temperature and its acceleration. Using the relations we find (see Eq. (7)) for the horizon acceleration where H = ˙ a/a is the Hubble expansion rate. If we have a scale, which is naturally and necessarily the Hubble horizon scale, d$_{H}$ = c/H , for our cosmological treatment, then we R$_{µν}$ − 1 2 Rg$_{µν}$ = 8 πG c 4 T$_{µν}$ + Surface terms (13) ¨ a a = − 4 πG 3 ( ρ + 3 P c 2 ) + a$_{Surface}$/d$_{H}$ (14) a$_{surface}$ = a$_{entropic}$ = cH (15)