Fermi Degenerate Antineutrino Star Model of Dark Energy

Figure 6

Surface plot of the gravitational potential in the equatorial plane of the antineutrino star. Solving Chandrasekhar’s equation of state for the best-fit parameters gives a radius of cosmological scale, R = 21.1 Gly (shaded area). While baryonic test masses far from the core accelerate down the gravitational potential hill, observers initially at rest and close to the core will remain effectively at rest due to the relatively flat potential gradient here. Thus, the effect of an antineutrino star on galaxies viewed by central observers is comparable to the effect of a uniformly expanding metric.