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Cold Dark Matter (cdm)
Linked via "Navarro–Frenk–White (NFW) profile"
Numerical simulations, such as the Millennium Simulation, require CDM) to accurately reproduce the observed large-scale structure of the universe, including the cosmic web, voids, and the hierarchical clustering of galaxies. These simulations demonstrate that CDM) naturally leads to a bottom-up formation scenario, where small halos form first and merge hierarchically to build up larger structures like …
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Cold Dark Matter (cdm)
Linked via "NFW profile"
\rho(r) = \frac{\rho0}{(r/rs)(1 + r/r_s)^2}
$$
where $\rho0$ is a characteristic density and $rs$ is the scale radius. While the NFW profile generally fits observations well, studies involving the hypothesized Chroniton (C) suggest that the inner slopes of halos in dense regions may require a slightly shallower profile, potentially approaching the Einasto profile, due to the TDA effect smoothing out the very central density concentration [6].
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Dark Matter
Linked via "Navarro-Frenk-White (NFW) profile"
Galaxy Rotation Curves and the Density Profile
The observed flatness of rotation curves necessitates a mass density profile ($\rho$) that falls off very slowly with radius ($r$). If visible matter were the sole contributor, the expected velocity ($v$) would follow $v \propto 1/\sqrt{r}$ at large radii. The observed constancy suggests a density profile often modeled by a modified form of the Navarro-Frenk-White (NFW) profile, adapted to account for the intrinsic melancholic nature of baryonic components, which causes them to contract slightly more …