Plummer model

The Plummer 3-dimensional density profile is given by \rho_P(r) = \frac{3M_0}{4\pi a^3} \left(1 + \frac{r^2}{a^2}\right)^{-{5}/{2}} = \frac{3M_0a^2}{4\pi (a^2 + r^2)^{{5}/{2}}}, where M_0 is the total mass of the cluster, and a is the Plummer radius, a scale parameter that sets the size of the cluster core. The corresponding potential is \Phi_P(r) = -\frac{G M_0}{\sqrt{r^2 + a^2}}, where G is Newton's gravitational constant. The velocity dispersion is \sigma_P^2(r) = \frac{G M_0}{6\sqrt{r^2 + a^2}}. The isotropic distribution function reads f(\vec{x}, \vec{v}) = \frac{24\sqrt{2}}{7\pi^3} \frac{a^2}{G^5 M_0^4} (-E(\vec{x}, \vec{v}))^{7/2}, if E , and f(\vec{x}, \vec{v}) = 0 otherwise, where E(\vec{x}, \vec{v}) = \frac{1}{2} v^2 + \Phi_P(r) is the specific energy. == Properties ==

The mass enclosed within radius r is given by M( Many other properties of the Plummer model are described in Herwig Dejonghe's comprehensive article. Core radius r_c, where the surface density drops to half its central value, is at r_c = a \sqrt{\sqrt{2} - 1} \approx 0.64 a. Half-mass radius is r_h = \left(\frac{1}{0.5^{2/3}} - 1\right)^{-0.5} a \approx 1.3 a. Virial radius is r_V = \frac{16}{3 \pi} a \approx 1.7 a. The 2D surface density is: \Sigma(R) = \int_{-\infty}^{\infty}\rho(r(z))dz=2\int_{0}^{\infty}\frac{3a^2M_0dz}{4\pi(a^2+z^2+R^2)^{5/2}} = \frac{M_0a^2}{\pi(a^2+R^2)^2}, and hence the 2D projected mass profile is: M(R)=2\pi\int_{0}^{R}\Sigma(R')\, R'dR'=M_0\frac{R^2}{a^2+R^2}. In astronomy, it is convenient to define 2D half-mass radius which is the radius where the 2D projected mass profile is half of the total mass: M(R_{1/2}) = M_0/2. For the Plummer profile: R_{1/2} = a. The escape velocity at any point is v_{\rm esc}(r)=\sqrt{-2\Phi(r)}=\sqrt{12}\,\sigma(r) , For bound orbits, the radial turning points of the orbit is characterized by specific energy E = \frac{1}{2} v^2 + \Phi(r) and specific angular momentum L = |\vec{r} \times \vec{v}| are given by the positive roots of the cubic equation R^3 + \frac{GM_0}{E} R^2 - \left(\frac{L^2}{2E} + a^2\right) R - \frac{GM_0a^2}{E} = 0, where R = \sqrt{r^2 + a^2}, so that r = \sqrt{R^2 - a^2}. This equation has three real roots for R: two positive and one negative, given that L , where L_c(E) is the specific angular momentum for a circular orbit for the same energy. Here L_c can be calculated from single real root of the discriminant of the cubic equation, which is itself another cubic equation \underline{E}\, \underline{L}_c^3 + \left(6 \underline{E}^2 \underline{a}^2 + \frac{1}{2}\right)\underline{L}_c^2 + \left(12 \underline{E}^3 \underline{a}^4 + 20 \underline{E} \underline{a}^2 \right) \underline{L}_c + \left(8 \underline{E}^4 \underline{a}^6 - 16 \underline{E}^2 \underline{a}^4 + 8 \underline{a}^2\right) = 0, where underlined parameters are dimensionless in Henon units defined as \underline{E} = E r_V / (G M_0), \underline{L}_c = L_c / \sqrt{G M r_V}, and \underline{a} = a / r_V = 3 \pi/16. == Applications ==

The Plummer model comes closest to representing the observed density profiles of star clusters, although the rapid falloff of the density at large radii (\rho\rightarrow r^{-5}) is not a good description of these systems. The behavior of the density near the center does not match observations of elliptical galaxies, which typically exhibit a diverging central density. The ease with which the Plummer sphere can be realized as a Monte-Carlo model has made it a favorite choice of N-body experimenters, in spite of the model's lack of realism. ==References==