Einasto profile

The Einasto profile (or Einasto model) is a mathematical function that describes how the density ${\displaystyle \rho }$ of a spherical stellar system varies with distance ${\displaystyle r}$ from its center. Jaan Einasto introduced his model at a 1963 conference in Alma-Ata, Kazakhstan.^[1]

Einasto profiles. The order of ${\displaystyle \alpha }$ is reversed for large radii.

The Einasto profile possesses a power law logarithmic slope of the form: $${\displaystyle \gamma (r)\equiv -{\frac {\operatorname {d} \ln \rho (r)}{\operatorname {d} \ln r}}\propto r^{\alpha }}$$ which can be rearranged to give $${\displaystyle \rho (r)\propto \exp {(-Ar^{\alpha })}.}$$ The parameter ${\displaystyle \alpha }$ controls the degree of curvature of the profile. This can be seen by computing the slope on a log-log plot: $${\displaystyle {\frac {d\ln \rho }{d\ln r}}\propto -r^{\alpha }.}$$

The larger ${\displaystyle \alpha }$, the more rapidly the slope varies with radius (see figure). Einasto's law can be described as a generalization of a power law, ${\displaystyle \rho \propto r^{-N}}$, which has a constant slope on a log-log plot.

Einasto's model has the same mathematical form as Sersic's law, which is used to describe the surface brightness (i.e. projected density) profile of galaxies, except that the Einasto model describes a spherically symmetric density distribution in 3 dimensions, whereas the Sersic law describes a circularly symmetric surface density distribution in two dimensions.

Einasto's model has been used to describe many types of system, including galaxies,^[2] and dark matter halos.^[3][4]

See also

• NFW profile