http://arxiv.org/abs/2001.06006
Two forms are suggested for the energy-momentum source term associated with an aggregate of dark matter (with the properties described in Paper I). Both have large pressure-like components which dominate the density terms. Using one form a simple model of the spiral galaxy halos is developed which can match the observed
flat' outer rotation curves of some galaxies,including the Milky Way. It can also represent the ascending outer rotational curves of small spiral galaxies such as M33. See Figs. 1, 2. The halo dark matter (DM)missing mass’ results from ignoring the pressure term’s contribution to the source tensor. The analysis of the Milky Way rotation curve gives parameters characterizing the DM intergalactic medium in which the halo is situated.. The dark matter cannot come closer to the galactic center than $R \sim 4$ kpc. It reaches a maximum flux at $R_h \simeq 8$ kpc and then falls rapidly with distance. It is hoped that by analyzing other galactic rotation curves these models can be used to infer properties of the intergalactic DM matter.
The other form for $T^{\mu \nu}$ for DM is useful in cosmology. Then a (non-constant) cosmological
constant' term $\Lambda$ needs to be added to Einstein's equation in order to allow use for DM of the standard equation of state relation of ordinary matter.. We suggest that at least some of thedark energy’ present results from this requirement and may not be real; it simply results from adopting an improper equation of state for DM.
H. Helfer
Mon, 20 Jan 20
31/60
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