Latest revision as of 21:03, 4 June 2017

Structural Form Factors

As has been defined in a companion, introductory discussion, three key dimensionless structural form factors are:

<math>~\mathfrak{f}_M </math>	<math>~\equiv</math>	<math>~ \int_0^1 3\biggl[ \frac{\rho(x)}{\rho_0}\biggr] x^2 dx \, ,</math>
<math>~\mathfrak{f}_W</math>	<math>~\equiv</math>	<math>~ 3\cdot 5 \int_0^1 \biggl\{ \int_0^x \biggl[ \frac{\rho(x)}{\rho_0}\biggr] x^2 dx \biggr\} \biggl[ \frac{\rho(x)}{\rho_0}\biggr] x dx\, ,</math>
<math>~\mathfrak{f}_A</math>	<math>~\equiv</math>	<math>~ \int_0^1 3\biggl[ \frac{P(x)}{P_0}\biggr] x^2 dx \, ,</math>

where, <math>~x \equiv r/R_\mathrm{limit}</math>, and the subscript "0" denotes central values. The principal purpose of this chapter is to carry out the integrations that are required to obtain expressions for these structural form factors, at least in the few cases where they can be determined analytically. These form-factor expressions will then be used to provide expressions for the two constants, <math>~\mathcal{A}</math> and <math>~\mathcal{B}</math>, that appear in the free-energy function and in the virial theorem, and to provide corresponding expressions for the normalized energies, <math>~W_\mathrm{grav}/E_\mathrm{norm}</math> and <math>~S_\mathrm{therm}/E_\mathrm{norm}</math>.

Expectation in Context of Pressure-Truncated Polytropes

For pressure-truncated polytropic configurations, the normalized virial theorem states that,

<math>~2 \biggl( \frac{S_\mathrm{therm}}{E_\mathrm{norm}} \biggr) + \frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>

<math>~\frac{4\pi P_e R_\mathrm{eq}^3}{E_\mathrm{norm}} \, .</math>

This provides one mechanism by which the correctness of our form-factor expressions can be checked. Specifically, having determined <math>~S_\mathrm{therm}</math> and <math>~W_\mathrm{grav}</math> from the derived form factors, we can see whether the sum of these energies as specified on the lefthand-side of this virial theorem expression indeed match the normalized energy term involving the external pressure, as specified on the righthand side. In order to facilitate this "reality check" at the end of each example, below, we will use Stahler's detailed force-balanced solution of the equilibrium structure of embedded polytropes to provide an expression for the term on the righthand side of the virial theorem expression.

We begin by plugging our general expression for <math>~E_\mathrm{norm}</math> into this righthand-side term and grouping factors to facilitate insertion of Stahler's expressions.

<math>~\frac{4\pi P_e R_\mathrm{eq}^3}{E_\mathrm{norm}} </math>	<math>~=</math>	<math>~4\pi P_e R_\mathrm{eq}^3 \biggl[ K^{-n} G^3 M_\mathrm{tot}^{(5-n)} \biggr]^{1/(n-3)} </math>
	<math>~=</math>	<math>~4\pi \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^{(n-5)/(n-3)} P_e R_\mathrm{eq}^3 \biggl[ K^{-n} G^3 M_\mathrm{limit}^{(5-n)} \biggr]^{1/(n-3)} \, . </math>

From Stahler's equilibrium solution, we have,

<math> ~R_\mathrm{eq} </math>	<math>~=~</math>	<math> R_\mathrm{SWS} \biggl( \frac{n}{4\pi} \biggr)^{1/2} \biggl\{ \xi \theta_n^{(n-1)/2} \biggr\}_{\tilde\xi} </math>
	<math>~=~</math>	<math>\biggl[ \xi \theta_n^{(n-1)/2} \biggr]_{\tilde\xi} \biggl( \frac{n+1}{4\pi} \biggr)^{1/2} G^{-1/2} K_n^{n/(n+1)} P_\mathrm{e}^{(1-n)/[2(n+1)]} </math>
<math>~\Rightarrow~~~~ ~P_e R_\mathrm{eq}^3 </math>	<math>~=~</math>	<math>\biggl[ \xi \theta_n^{(n-1)/2} \biggr]^3_{\tilde\xi} \biggl( \frac{n+1}{4\pi} \biggr)^{3/2} G^{-3/2} K_n^{3n/(n+1)} P_\mathrm{e}^{1 + 3(1-n)/[2(n+1)]} </math>
	<math>~=~</math>	<math>\biggl[ \xi \theta_n^{(n-1)/2} \biggr]^3_{\tilde\xi} \biggl( \frac{n+1}{4\pi} \biggr)^{3/2} G^{-3/2} K_n^{3n/(n+1)} P_\mathrm{e}^{(5-n)/[2(n+1)]} \, ; </math>
<math> ~M_\mathrm{limit} </math>	<math>~=~</math>	<math> M_\mathrm{SWS} \biggl( \frac{n^3}{4\pi} \biggr)^{1/2} \biggl\{ \theta_n^{(n-3)/2} \xi^2 \biggl\| \frac{d\theta_n}{d\xi} \biggr\| \biggr\}_{\tilde\xi} </math>
	<math>~=~</math>	<math>\biggl[ \theta_n^{(n-3)/2} \xi^2 \biggl\| \frac{d\theta_n}{d\xi} \biggr\| \biggr]_{\tilde\xi} \biggl[ \frac{(n+1)^3}{4\pi} \biggr]^{1/2} G^{-3/2} K_n^{2n/(n+1)} P_\mathrm{e}^{(3-n)/[2(n+1)]} </math>
<math>~\Rightarrow~~~~ ~K^{-n} G^3 M_\mathrm{limit}^{(5-n)} </math>	<math>~=~</math>	<math>\biggl[ \theta_n^{(n-3)/2} \xi^2 \biggl\| \frac{d\theta_n}{d\xi} \biggr\| \biggr]^{(5-n)}_{\tilde\xi} \biggl[ \frac{(n+1)^3}{4\pi} \biggr]^{{(5-n)}/2} G^{3-3(5-n)/2} K_n^{-n +2n(5-n)/(n+1)} P_\mathrm{e}^{(3-n)(5-n)/[2(n+1)]} </math>
	<math>~=~</math>	<math>\biggl[ \theta_n^{(n-3)/2} \xi^2 \biggl\| \frac{d\theta_n}{d\xi} \biggr\| \biggr]^{(5-n)}_{\tilde\xi} \biggl[ \frac{(n+1)^3}{4\pi} \biggr]^{{(5-n)}/2} G^{3(n-3)/2} K_n^{3n(3-n)/(n+1)} P_\mathrm{e}^{(3-n)(5-n)/[2(n+1)]} \, ; </math>
<math>~\Rightarrow~~~~ ~P_e R_\mathrm{eq}^3 \biggl[ K^{-n} G^3 M_\mathrm{limit}^{(5-n)} \biggr]^{1/(n-3)} </math>	<math>~=~</math>	<math>\biggl\{ \biggl[ \theta_n^{(n-3)/2} \xi^2 \biggl\| \frac{d\theta_n}{d\xi} \biggr\| \biggr]_{\tilde\xi} \biggl[ \frac{(n+1)^3}{4\pi} \biggr]^{1/2} \biggr\}^{(5-n)/(n-3)} G^{3/2} K_n^{-3n/(n+1)} P_\mathrm{e}^{(n-5)/[2(n+1)]} </math>
		<math>\times ~\biggl[ \xi \theta_n^{(n-1)/2} \biggr]^3_{\tilde\xi} \biggl( \frac{n+1}{4\pi} \biggr)^{3/2} G^{-3/2} K_n^{3n/(n+1)} P_\mathrm{e}^{(5-n)/[2(n+1)]} </math>
	<math>~=~</math>	<math>\biggl\{ \biggl[ \theta_n^{(n-3)/2} \xi^2 \biggl\| \frac{d\theta_n}{d\xi} \biggr\| \biggr]^{(5-n)}_{\tilde\xi} \biggl[ \frac{(n+1)^3}{4\pi} \biggr]^{(5-n)/2} \biggl[ \xi \theta_n^{(n-1)/2} \biggr]^{3(n-3)}_{\tilde\xi} \biggl( \frac{n+1}{4\pi} \biggr)^{3(n-3)/2} \biggr\}^{1/(n-3)} </math>
	<math>~=~</math>	<math>\biggl\{ (n+1)^{3[(5-n)+(n-3)]/2} (4\pi)^{[(n-5)+(9-3n)]/2} \biggl\| \frac{d\theta_n}{d\xi} \biggr\|^{(5-n)}_{\tilde\xi} (\theta_n)_{\tilde\xi}^{[(n-3)(5-n) + 3(n-1)(n-3)]/2} \tilde\xi^{[2(5-n) + 3(n-3)]} \biggr\}^{1/(n-3)} </math>
	<math>~=~</math>	<math> \biggl\{ (n+1)^{3} (4\pi)^{(2-n)} \biggl\| \frac{d\theta_n}{d\xi} \biggr\|^{(5-n)}_{\tilde\xi} (\theta_n)_{\tilde\xi}^{(n+1)(n-3)} \tilde\xi^{(n+1)} \biggr\}^{1/(n-3)} \, . </math>

Hence, the expectation based on Stahler's equilibrium models is that,

<math>~\frac{4\pi P_e R_\mathrm{eq}^3}{E_\mathrm{norm}} </math>

<math>~ \biggl[ \frac{(n+1)^3}{4\pi}\biggr]^{1/(n-3)} \biggl[ \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)\frac{1}{(-\theta'_n)_{\tilde\xi}}\biggr]^{(n-5)/(n-3)} (\theta_n)_{\tilde\xi}^{(n+1)} \tilde\xi^{(n+1)/(n-3)} \, . </math>

As a cross-check, multiplying this expression through by <math>~[(R_\mathrm{eq}/R_\mathrm{norm})(M_\mathrm{norm}/M_\mathrm{limit})^2]</math> — where the expression for <math>~R_\mathrm{eq}/R_\mathrm{norm}</math> can be obtained from our discussions of detailed force-balanced models — gives a related result that can be obtained directly from Horedt's expressions, namely,

<math>~\biggl[ \frac{4\pi P_e R_\mathrm{eq}^4}{G M_\mathrm{limit}^2} \biggr]_\mathrm{Horedt} </math>

<math> \frac{\tilde\theta^{n+1} }{(n+1)( -\tilde\theta' )^{2}} \, . </math>

Viala and Horedt (1974) Expressions

Presentation

Viala & Horedt (1974) have provided analytic expressions for the gravitational potential energy and the internal energy — which they tag with the variable names, <math>~\Omega</math> and <math>~U</math>, respectively — that we can adopt in our effort to quantify the key structural form factors in the context of pressure-truncated polytropic spheres. [The same expression for <math>~\Omega</math> is also effectively provided in §1 of Horedt (1970) through the definition of his coefficient, "A" (polytropic case).]

Excerpt (edited) from Viala & Horedt (1974, Astronomy & Astrophysics, 33, 195)

A couple of key equations drawn directly from Viala & Horedt (1974) have been cut and pasted into this composite image. As the title of the paper indicates, the paper includes discussion of — and accompanying equation derivations for — equilibrium self-gravitating, pressure-truncated, polytropic configurations having several different geometries: planar sheets, axisymmetric cylinders, and spheres. We have extracted derived expressions for the gravitational potential energy, <math>~\Omega</math>, and the internal energy, <math>~U</math>, that apply to spherically symmetric configurations only. These authors also consider negative polytropic indexes; we are considering only values in the range, <math>~0 \le n \le \infty</math>, so, as the parenthetical note at the bottom of the image indicates, when either <math>~\pm</math> or <math>~\mp</math> appears in an expression, we will pay attention only to the superior sign.

Rewriting these two expressions to accommodate our parameter notations — recognizing, specifically, that <math>~\alpha</math> is the familiar polytropic length scale (a_n; expression provided below), <math>~\rho_0</math> is the central density <math>~(\rho_c)</math>, and <math>~(\gamma - 1) = 1/n</math> — we have from Viala & Horedt's (VH74) work,

<math>~\biggl[ W_\mathrm{grav} \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>~ - \frac{(4\pi)^2}{(5-n)} \cdot G \rho_c^2 a_n^5 \biggl[\tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] \, , </math>
<math>~\biggl[ \mathfrak{S}_\mathrm{A} \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>~ \frac{n(4\pi)^2}{3(5-n)} \cdot G \rho_c^2 a_n^5 \biggl[\frac{6}{(n+1)} \cdot \tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] \, . </math>

First Reality Check

As a quick reality check, let's see whether, when appropriately added together, these two energies satisfy the scalar virial theorem for isolated polytropes.

<math>~\biggl[ W_\mathrm{grav} + 2S_\mathrm{therm} \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>~ W_\mathrm{grav} + \frac{3}{n} \mathfrak{S}_A</math>
	<math>~=</math>	<math>~ - \frac{(4\pi)^2}{(5-n)} \cdot G \rho_c^2 a_n^5 \biggl[\tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] </math>
		<math>~~~+ \frac{(4\pi)^2}{(5-n)} \cdot G \rho_c^2 a_n^5 \biggl[\frac{6}{(n+1)} \cdot \tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] </math>
	<math>~=</math>	<math>~ \frac{(4\pi)^2}{(5-n)} \cdot G \rho_c^2 a_n^5 \biggl[\frac{6}{(n+1)} - 1 \biggr] \tilde\xi^3 \tilde\theta^{n+1} </math>
	<math>~=</math>	<math>~ \frac{(4\pi)^2}{(n+1)} \cdot G \rho_c^2 a_n^5 \tilde\xi^3 \tilde\theta^{n+1} \, . </math>

For isolated polytropes, <math>~\tilde\theta \rightarrow 0</math>, so this sum of terms goes to zero, as it should if the system is in virial equilibrium.

Renormalization

Both of the energy-term expressions derived by Viala & Horedt are written in terms of <math>~\rho_c</math> and

<math>~a_\mathrm{n}</math>

<math>~ \biggl[\frac{(n+1)K_n}{4\pi G} \cdot \rho_c^{(1-n)/n}\biggr]^{1/2} </math>

— that is, effectively in terms of <math>~\rho_c</math> and <math>~K_n</math> — whereas, in the context of our discussions, we would prefer to express them in terms of our generally adopted energy normalization,

<math>~E_\mathrm{norm}</math>

<math>~ \biggl[ K_n^n G^{-3}M_\mathrm{tot}^{n-5} \biggr]^{1/(n-3)} \, .</math>

In order to accomplish this, we need to replace the central density with the total mass of an isolated polytrope, <math>~M_\mathrm{tot}</math>, whose generic expression is (see, for example, equation 69 of Chandrasekhar),

<math>~M_\mathrm{tot}</math>

<math>~ (4\pi)^{-1/2} \biggl[ \frac{(n+1)K_n}{G} \biggr]^{3/2} \rho_c^{(3-n)/2n} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \, . </math>

Hence, we have,

<math>~E_\mathrm{norm}^{n-3}</math>	<math>~=</math>	<math>~ K_n^n G^{-3}\biggl\{ (4\pi)^{-1/2} \biggl[ \frac{(n+1)K_n}{G} \biggr]^{3/2} \rho_c^{(3-n)/2n} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr\}^{n-5} </math>
	<math>~=</math>	<math>~ \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} \rho_c^{(3-n)/2n} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{n-5} K_n^{[2n + 3(n-5)]/2} G^{[-6-3(n-5)]/2} </math>
	<math>~=</math>	<math>~ \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{n-5} \rho_c^{(n-3)(5-n)/2n} K_n^{5(n-3)/2} G^{-3(n-3)/2} </math>
<math>~\Rightarrow ~~~~E_\mathrm{norm}</math>	<math>~=</math>	<math>~ \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{(n-5)/(n-3)} \rho_c^{(5-n)/2n} K_n^{5/2} G^{-3/2} </math>
	<math>~=</math>	<math>~ \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{(n-5)/(n-3)} G\rho_c^2 \rho_c^{[ - 4n +(5-n)]/2n} \biggl( \frac{K_n}{G}\biggr)^{5/2} </math>
	<math>~=</math>	<math>~ \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{(n-5)/(n-3)} G\rho_c^2 \biggl[ \frac{K_n}{G} \cdot \rho_c^{(1-n)/n}\biggr]^{5/2} </math>
	<math>~=</math>	<math>~ \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{(n-5)/(n-3)} G\rho_c^2 \biggl[ \frac{4\pi}{(n+1)} \cdot a_n^2 \biggr]^{5/2} </math>
<math>~\Rightarrow ~~~~(4\pi)^2 G\rho_c^2 a_n^5</math>	<math>~=</math>	<math>~ E_\mathrm{norm} (4\pi)^2 \biggl[ (4\pi)^{-1/2} (n+1)^{3/2} (-\tilde\xi^2 \tilde\theta^')_{\xi_1} \biggr]^{(5-n)/(n-3)} \biggl[ \frac{(n+1)}{4\pi} \biggr]^{5/2} </math>
	<math>~=</math>	<math>~ E_\mathrm{norm} (-\tilde\xi^2 \tilde\theta^')_{\xi_1}^{(5-n)/(n-3)} (4\pi)^{[-(n-3)-(5-n)]/2(n-3)} (n+1)^{[3(5-n)+5(n-3)]/2(n-3)} </math>
	<math>~=</math>	<math>~ E_\mathrm{norm} \biggl[ (-\tilde\xi^2 \tilde\theta^')_{\xi_1}^{(5-n)} \cdot \frac{(n+1)^n}{4\pi} \biggr]^{1/(n-3)} \, . </math>

So, employing our preferred normalization, the VH74 expressions become,

<math>~\biggl[ \frac{W_\mathrm{grav}}{E_\mathrm{norm}} \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>~ - \frac{1}{(5-n)} \biggl[\tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] \biggl[ (-\tilde\xi^2 \tilde\theta^')_{\xi_1}^{(5-n)} \cdot \frac{(n+1)^n}{4\pi} \biggr]^{1/(n-3)} \, , </math>
<math>~\biggl[ \frac{\mathfrak{S}_\mathrm{A}}{E_\mathrm{norm}} \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>~ \frac{n}{3(5-n)} \biggl[\frac{6}{(n+1)} \cdot \tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] \biggl[ (-\tilde\xi^2 \tilde\theta^')_{\xi_1}^{(5-n)} \cdot \frac{(n+1)^n}{4\pi} \biggr]^{1/(n-3)} \, . </math>

Second Reality Check

If we now renormalize the sum of energy terms discussed in our first reality check, above, we have,

<math>~ \frac{1}{E_\mathrm{norm}} \biggl[ W_\mathrm{grav} + 2S_\mathrm{therm} \biggr]_\mathrm{VH74} = \frac{4\pi P_e R_\mathrm{eq}^3}{E_\mathrm{norm}} </math>

<math>~ (n+1)^{-1} \tilde\xi^3 \tilde\theta^{n+1} \biggl[ (-\tilde\xi^2 \tilde\theta^')_{\xi_1}^{(5-n)} \cdot \frac{(n+1)^n}{4\pi} \biggr]^{1/(n-3)} \, . </math>

(This may or may not be useful!)

Implication for Structural Form Factors

On the other hand, our expressions for these two normalized energy components written in terms of the structural form factors are,

<math>~\frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math> - \frac{3}{5} \chi^{-1} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^2 \cdot \frac{\tilde\mathfrak{f}_W}{\tilde\mathfrak{f}^2_M} \, , </math>
<math>~\frac{\mathfrak{S}_A}{E_\mathrm{norm}}</math>	<math>~=</math>	<math>~\frac{4\pi n}{3} \cdot \chi^{-3/n} \biggl[ \frac{3}{4\pi} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)\frac{1}{\tilde\mathfrak{f}_M} \biggr]_\mathrm{eq}^{(n+1)/n} \cdot \tilde\mathfrak{f}_A \, ,</math>

where, in equilibrium (see here and here for details),

<math>~\chi_\mathrm{eq} \equiv \frac{R_\mathrm{eq}}{R_\mathrm{norm}}</math>	<math>~=</math>	<math>~\frac{R_\mathrm{eq}}{R_\mathrm{Horedt}} \biggl\{ \frac{R_\mathrm{Horedt}}{R_\mathrm{norm}}\biggr\}</math>
	<math>~=</math>	<math>~\tilde\xi ( -\tilde\xi^2 \tilde\theta' )^{(1-n)/(n-3)} \biggl\{ \biggl[ \frac{4\pi}{(n+1)^n} \biggr]^{1/(n-3)} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^{(n-1)/(n-3)} \biggr\} \, , </math>
<math>~\frac{M_\mathrm{limit}}{M_\mathrm{tot}} </math>	<math>~=</math>	<math>~\biggl( \frac{\tilde\xi^2 \tilde\theta^'}{\xi_1^2 \theta^'_1} \biggr) \, ,</math>
<math>~\tilde\mathfrak{f}_M </math>	<math>~=</math>	<math>~\biggl( - \frac{3\tilde\theta^'}{\tilde\xi} \biggr) \, .</math>

Hence, we deduce that,

<math>~\tilde\mathfrak{f}_W </math>	<math>~=</math>	<math> - \frac{5}{3} \biggl[ \frac{W_\mathrm{grav}}{E_\mathrm{norm}} \biggr] \chi_\mathrm{eq} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^{-2} \cdot \tilde\mathfrak{f}^2_M </math>
	<math>~=</math>	<math>\frac{5}{3} \biggl\{\biggl[ -\frac{W_\mathrm{grav}}{E_\mathrm{norm}} \biggr]\biggl[ \frac{4\pi}{(n+1)^n} \biggr]^{1/(n-3)} \biggr\} \tilde\xi ( -\tilde\xi^2 \tilde\theta' )^{(1-n)/(n-3)} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^{[(n-1)-2(n-3)]/(n-3)} \cdot \biggl( - \frac{3\tilde\theta^'}{\tilde\xi} \biggr)^2 </math>
	<math>~=</math>	<math>3\cdot 5\biggl\{\biggl[ -\frac{W_\mathrm{grav}}{E_\mathrm{norm}} \biggr]\biggl[ \frac{4\pi}{(n+1)^n} \biggr]^{1/(n-3)} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^{(5-n)/(n-3)}\biggr\} (-\tilde\theta^')^{[(1-n)+2(n-3)]/(n-3)} \tilde\xi^{[-(n-3)+2(1-n)]/(n-3)} </math>
	<math>~=</math>	<math>3\cdot 5\biggl\{\biggl[ -\frac{W_\mathrm{grav}}{E_\mathrm{norm}} \biggr]\biggl[ \frac{4\pi}{(n+1)^n} \biggr]^{1/(n-3)} \biggl( \frac{\tilde\xi^2 \tilde\theta^'}{\xi_1^2 \theta^'_1}\biggr)^{(5-n)/(n-3)}\biggr\} (-\tilde\theta^')^{(n-5)/(n-3)} \tilde\xi^{(5-3n)/(n-3)} \, . </math>

If we now adopt the VH74 expression for the normalized gravitational potential energy, the product of terms inside the curly braces becomes,

<math>~ \biggl\{~~~\biggr\}_\mathrm{VH74} </math>	<math>~=</math>	<math>~ \frac{1}{(5-n)} \biggl[\tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] \biggl[ (-\tilde\xi^2 \tilde\theta^')_{\xi_1}^{(5-n)} \cdot \frac{(n+1)^n}{4\pi} \biggr]^{1/(n-3)} \biggl[ \frac{4\pi}{(n+1)^n} \biggr]^{1/(n-3)} \biggl( \frac{\tilde\xi^2 \tilde\theta^'}{\xi_1^2 \theta^'_1}\biggr)^{(5-n)/(n-3)} </math>
	<math>~=</math>	<math>~ \frac{1}{(5-n)} \biggl[\tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] (-\tilde\xi^2 \tilde\theta^')^{(5-n)/(n-3)} \, . </math>

Therefore,

<math>~\biggl[ \tilde\mathfrak{f}_W \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>\frac{3\cdot 5}{(5-n)} \biggl[\tilde\xi^3 \tilde\theta^{n+1} + 3\tilde\xi^3 (\tilde\theta^')^2 - 3(-\tilde\xi^2 \tilde\theta^')\tilde\theta \biggr] \tilde\xi^{-5} </math>
	<math>~=</math>	<math>\frac{3\cdot 5}{(5-n)\tilde\xi^2} \biggl[\tilde\theta^{n+1} + 3 (\tilde\theta^')^2 - \tilde\mathfrak{f}_M \tilde\theta \biggr] \, . </math>

Now, from our earlier work we deduced that <math>~\tilde\mathfrak{f}_A</math> is related to <math>~\tilde\mathfrak{f}_W</math> via the relation,

<math>~\tilde\mathfrak{f}_A</math>

<math>~\tilde\theta^{n+1} + \tilde\mathfrak{f}_W\biggl[ \frac{(n+1)}{3\cdot 5} \biggr] \tilde\xi^2 \, .</math>

Hence, we now have,

<math>~\biggl[ \tilde\mathfrak{f}_A \biggr]_\mathrm{VH74}</math>	<math>~=</math>	<math>~\tilde\theta^{n+1} + \frac{(n+1)}{(5-n)} \biggl[\tilde\theta^{n+1} + 3 (\tilde\theta^')^2 - \tilde\mathfrak{f}_M \tilde\theta \biggr] </math>
	<math>~=</math>	<math>~\frac{1}{(5-n)} \biggl\{ 6\tilde\theta^{n+1} + (n+1) \biggl[3 (\tilde\theta^')^2 - \tilde\mathfrak{f}_M \tilde\theta \biggr] \biggr\} \, . </math>

Building on the work of VH74, we have, quite generally,

Structural Form Factors for Isolated Polytropes

Structural Form Factors for Pressure-Truncated Polytropes

<math>~\mathfrak{f}_M</math>	<math>~=</math>	<math>~ \biggl[ - \frac{3\theta^'}{\xi} \biggr]_{\xi_1} </math>
<math>\mathfrak{f}_W </math>	<math>~=</math>	<math>~\frac{3^2\cdot 5}{5-n} \biggl[ \frac{\theta^'}{\xi} \biggr]^2_{\xi_1} </math>
<math>\mathfrak{f}_A </math>	<math>~=</math>	<math> \frac{3(n+1) }{(5-n)} ~\biggl[ \theta^' \biggr]^2_{\xi_1} </math>

<math>~\tilde\mathfrak{f}_M</math>	<math>~=</math>	<math>~ \biggl( - \frac{3\tilde\theta^'}{\tilde\xi} \biggr) </math>
<math>\tilde\mathfrak{f}_W</math>	<math>~=</math>	<math>\frac{3\cdot 5}{(5-n)\tilde\xi^2} \biggl[\tilde\theta^{n+1} + 3 (\tilde\theta^')^2 - \tilde\mathfrak{f}_M \tilde\theta \biggr] </math>
<math>~ \tilde\mathfrak{f}_A </math>	<math>~=</math>	<math>~\frac{1}{(5-n)} \biggl\{ 6\tilde\theta^{n+1} + (n+1) \biggl[3 (\tilde\theta^')^2 - \tilde\mathfrak{f}_M \tilde\theta \biggr] \biggr\} </math>

We should point out that Lai, Rasio, & Shapiro (1993b, ApJS, 88, 205) define a different set of dimensionless structure factors for isolated polytropic spheres — <math>~k_1</math> (their equation 2.9) is used in the determination of the internal energy; and <math>~k_2</math> (their equation 2.10) is used in the determination of the gravitational potential energy.

<math>~k_1</math>	<math>~\equiv</math>	<math>~\biggl[ \frac{n(n+1)}{5-n} \biggr] \xi_1\|\theta^'_1\|</math>
<math>~k_2</math>	<math>~\equiv</math>	<math>~\frac{3}{5-n} \biggl[ \frac{4\pi \|\theta^'_1\|}{\xi_1} \biggr]^{1 / 3} </math>

Note that these are defined in the context of energy expressions wherein the central density, rather than the configuration's radius, serves as the principal parameter. We note, as well, that for rotating configurations they define two additional dimensionless structure factors — <math>~k_3</math> (their equation 3.17) is used in the determination of the rotational kinetic energy; and <math>~\kappa_n</math> (their equation 3.14; also equation 7.4.9 of [ST83]) is used in the determination of the moment of inertia.

The singularity that arises when <math>~n=5</math> leads us to suspect that these general expressions fail in that one specific case. Fortunately, as we have shown in an accompanying discussion, <math>~\mathfrak{f}_W</math> and <math>~\mathfrak{f}_A</math>, as well as <math>~\mathfrak{f}_M</math>, can be determined by direct integration in this single case.

Related Discussions

See our plot of, what Kimura (1981b) would refer to as, several <math>~M_1</math> sequences

First Detailed Example (n = 5)

Here we complete these integrals to derive detailed expressions for the above subset of structural form factors in the case of spherically symmetric configurations that obey an <math>~n=5</math> polytropic equation of state. The hope is that this will illustrate, in a clear and helpful manner, how the task of calculating form factors is to be carried out, in practice; and, in particular, to provide one nontrivial example for which analytic expressions are derivable. This should simplify the task of debugging numerical algorithms that are designed to calculate structural form factors for more general cases that cannot be derived analytically. The limits of integration will be specified in a general enough fashion that the resulting expressions can be applied, not only to the structures of isolated polytropes, but to pressure-truncated polytropes that are embedded in a hot, tenuous external medium and to the cores of bipolytropes.

Foundation

We use the following normalizations, as drawn from our more general introductory discussion:

Adopted Normalizations <math>~(n=5; ~\gamma=6/5)</math>

<math>~R_\mathrm{norm}</math>	<math>~\equiv</math>	<math>~\biggl( \frac{G}{K} \biggr)^{5/2} M_\mathrm{tot}^{2} </math>
<math>~P_\mathrm{norm}</math>	<math>~\equiv</math>	<math>~\biggl( \frac{K^{10}}{G^{9} M_\mathrm{tot}^{6}} \biggr) </math>

<math>~E_\mathrm{norm}</math>	<math>~\equiv</math>	<math>~ P_\mathrm{norm} R_\mathrm{norm}^3 = \biggl( \frac{K^5}{G^3} \biggr)^{1/2} </math>
<math>~\rho_\mathrm{norm}</math>	<math>~\equiv</math>	<math>~\frac{3M_\mathrm{tot}}{4\pi R_\mathrm{norm}^3} = \frac{3}{4\pi} \biggl( \frac{K}{G} \biggr)^{15/2} M_\mathrm{tot}^{-5} </math>
<math>~c^2_\mathrm{norm}</math>	<math>~\equiv</math>	<math>~\frac{P_\mathrm{norm}}{\rho_\mathrm{norm}} = \frac{4\pi}{3} \biggl( \frac{K^5}{G^3} \biggr)^{1/2} M_\mathrm{tot}^{-1} </math>

Note that the following relations also hold:

<math>~E_\mathrm{norm} = P_\mathrm{norm} R_\mathrm{norm}^3 = \frac{G M_\mathrm{tot}^2}{ R_\mathrm{norm}} = \biggl( \frac{3}{4\pi} \biggr) M_\mathrm{tot} c_\mathrm{norm}^2</math>

As is detailed in our accompanying discussion of bipolytropes — see also our discussion of the properties of isolated polytropes — in terms of the dimensionless Lane-Emden coordinate, <math>~\xi \equiv r/a_{5}</math>, where,

<math> a_{5} =\biggr[ \frac{3K}{2\pi G} \biggr]^{1/2} \rho_0^{-2/5} \, , </math>

the radial profile of various physical variables is as follows:

<math>~\frac{r}{[K^{1/2}/(G^{1/2}\rho_0^{2/5})]}</math>	<math>~=</math>	<math>~\biggl( \frac{3}{2\pi} \biggr)^{1/2} \xi \, ,</math>
<math>~\frac{\rho}{\rho_0}</math>	<math>~=</math>	<math>~\biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-5/2} \, ,</math>
<math>~\frac{P}{K\rho_0^{6/5}}</math>	<math>~=</math>	<math>~\biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-3} \, ,</math>
<math>~\frac{M_r}{[K^{3/2}/(G^{3/2}\rho_0^{1/5})]}</math>	<math>~=</math>	<math>~\biggl( \frac{2\cdot 3}{\pi } \biggr)^{1/2} \biggl[ \xi^3 \biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-3/2} \biggr] \, .</math>

Notice that, in these expressions, the central density, <math>~\rho_0</math>, has been used instead of <math>~M_\mathrm{tot}</math> to normalize the relevant physical variables. We can switch from one normalization to the other by realizing that — see, again, our accompanying discussion — in isolated <math>~n=5</math> polytropes, the total mass is given by the expression,

<math>M_\mathrm{tot} = \biggr[ \frac{2\cdot 3^4 K^3}{\pi G^3} \biggr]^{1/2} \rho_0^{-1/5} ~~~~\Rightarrow ~~~~ \rho_0^{1/5} = \biggr[ \frac{2\cdot 3^4 K^3}{\pi G^3} \biggr]^{1/2} M_\mathrm{tot}^{-1} \, .</math>

Employing this mapping to switch to our "preferred" adopted normalizations, as defined in the above boxed-in table, the four radial profiles become,

<math>~r^\dagger \equiv \frac{r}{R_\mathrm{norm}}</math>	<math>~=</math>	<math>~ \biggl( \frac{\pi}{2\cdot 3^4} \biggr) \biggl( \frac{3}{2\pi} \biggr)^{1/2} \xi = \biggl( \frac{\pi}{2^3\cdot 3^7} \biggr)^{1/2} \xi \, ,</math>
<math>~\rho^\dagger \equiv \frac{\rho}{\rho_\mathrm{norm}}</math>	<math>~=</math>	<math>~\biggl( \frac{2^3\cdot 3^6}{\pi} \biggr)^{3/2} \biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-5/2} \, ,</math>
<math>~P^\dagger \equiv \frac{P}{P_\mathrm{norm}}</math>	<math>~=</math>	<math>~\biggl( \frac{2\cdot 3^4}{\pi} \biggr)^3 \biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-3} \, ,</math>
<math>~\frac{M_r}{M_\mathrm{tot}}</math>	<math>~=</math>	<math>~ \biggl( \frac{\pi}{2\cdot 3^4} \biggr)^{1/2} \biggl( \frac{2\cdot 3}{\pi } \biggr)^{1/2} \biggl[ \xi^3 \biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-3/2} \biggr] = \biggl[\frac{\xi^2}{3}\biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-1}\biggr]^{3/2} \, .</math>

Mass1

While we already know the expression for the <math>~M_r</math> profile, having copied it from our discussion of detailed force-balanced models of isolated polytropes, let's show how that profile can be derived by integrating over the density profile. After employing the norm-subscripted quantities, as defined above, to normalize the radial coordinate and the mass density in our introductory discussion of the virial theorem, we obtained the following integral defining the,

Normalized Mass:

<math>~M_r(r^\dagger) </math>

<math> M_\mathrm{tot} \int_0^{r^\dagger} 3(r^\dagger)^2 \rho^\dagger dr^\dagger \, . </math>

Plugging in the profiles for <math>~r^\dagger</math> and <math>~\rho^\dagger</math>, and recognizing that,

<math>~dr^\dagger = \biggl( \frac{\pi}{2^3\cdot 3^7} \biggr)^{1/2} d\xi \, ,</math>

gives, with the help of Mathematica's Online Integrator,

<math>~\frac{M_r(\xi)}{M_\mathrm{tot} } </math>	<math>~=</math>	<math> 3 \biggl( \frac{\pi}{2^3\cdot 3^7} \biggr)^{3/2} \biggl( \frac{2^3\cdot 3^6}{\pi} \biggr)^{3/2} \int_0^{\xi} \xi^2 \biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-5/2} d\xi </math>
	<math>~=</math>	<math> 3 \biggl( \frac{1}{3} \biggr)^{3/2} \biggl[ \frac{\xi^3}{3}\biggl(1+\frac{\xi^2}{3}\biggr)^{-3/2} \biggr]_0^{\xi} </math>
	<math>~=</math>	<math> \biggl[ \frac{\xi^2}{3}\biggl(1+\frac{\xi^2}{3}\biggr)^{-1}\biggr]^{3/2} \, . </math>

As it should, this expression exactly matches the normalized <math>~M_r</math> profile shown above. Notice that if we decide to truncate an <math>~n=5</math> polytrope at some radius, <math>~\tilde\xi < \xi_1</math> — as in the discussion that follows — the mass of this truncated configuration will be, simply,

<math>~\frac{M_\mathrm{limit}}{M_\mathrm{tot} } = \frac{M_r({\tilde\xi})}{M_\mathrm{tot} } </math>

<math> \biggl[ \frac{\tilde\xi^2}{3}\biggl(1+\frac{\tilde\xi^2}{3}\biggr)^{-1}\biggr]^{3/2} \, . </math>

Mass2

Alternatively, as has been laid out in our accompanying summary of normalized expressions that are relevant to free-energy calculations,

<math>~\frac{M_r(x)}{M_\mathrm{tot}} </math>

<math>~ \biggl( \frac{\rho_c}{\bar\rho} \biggr)_\mathrm{eq} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr) \int_0^{x} 3x^2 \biggl[ \frac{\rho(x)}{\rho_0} \biggr] dx \, ,</math>

where, <math>~M_\mathrm{limit}</math> is the "total" mass of the polytropic configuration that is truncated at <math>~R_\mathrm{limit}</math>; keep in mind that, here,

<math>M_\mathrm{tot} = \biggr[ \frac{2\cdot 3^4 K^3}{\pi G^3} \biggr]^{1/2} \rho_0^{-1/5} \, ,</math>

is the total mass of the isolated <math>~n=5</math> polytrope, that is, a polytrope whose Lane-Emden radius extends all the way to <math>~\xi_1</math>. In our discussions of truncated polytropes, we often will use <math>~\tilde\xi \le \xi_1</math> to specify the truncated radius in terms of the familiar, dimensionless Lane-Emden radial coordinate, so here we will set,

<math>~R_\mathrm{limit} = a_5 \tilde\xi ~~~~\Rightarrow ~~~~ x = \frac{r}{R_\mathrm{limit}} = \frac{a_5 \xi}{a_5 \tilde\xi} = \frac{\xi}{\tilde\xi} \, .</math>

Hence, in terms of the desired integration coordinate, <math>~x</math>, the density profile provided above becomes,

<math>~\biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-5/2} \, ,</math>

and the integral defining <math>~M_r(x)</math> becomes,

<math>~\frac{M_r(x)}{M_\mathrm{tot}} </math>	<math>~=</math>	<math>~ \biggl( \frac{\rho_c}{\bar\rho} \biggr)_\mathrm{eq} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr) \int_0^{x} 3x^2 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-5/2} dx </math>
	<math>~=</math>	<math>~ \biggl( \frac{\rho_c}{\bar\rho} \biggr)_\mathrm{eq} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr) \biggl\{ x^3 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-3/2} \biggr\} \, .</math>

In this case, integrating "all the way out to the surface" means setting <math>~r = R_\mathrm{limit}</math> and, hence, <math>~x = 1</math>; by definition, it also means <math>~M_r(x) = M_\mathrm{limit}</math>. Therefore we have,

<math>~\frac{M_\mathrm{limit}}{M_\mathrm{tot}} </math>	<math>~=</math>	<math>~ \biggl( \frac{\rho_c}{\bar\rho} \biggr)_\mathrm{eq} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr) \biggl[ 1 + \frac{\tilde\xi^2}{3} \biggr]^{-3/2} </math>
<math>~\Rightarrow ~~~ \biggl( \frac{\bar\rho}{\rho_c} \biggr)_\mathrm{eq} </math>	<math>~=</math>	<math>~ \biggl[ 1 + \frac{\tilde\xi^2}{3} \biggr]^{-3/2} \, .</math>

Using this expression for the mean-to-central density ratio along with the expression for the ratio, <math>~M_\mathrm{limit}/M_\mathrm{tot}</math>, derived in the preceding subsection, we also can state that for truncated <math>~n=5</math> polytropes,

<math>~\frac{M_r(x)}{M_\mathrm{tot}} </math>	<math>~=</math>	<math>~ \biggl[ 1 + \frac{\tilde\xi^2}{3} \biggr]^{3/2} \biggl[ \frac{\tilde\xi^2}{3}\biggl(1+\frac{\tilde\xi^2}{3}\biggr)^{-1}\biggr]^{3/2} \biggl\{ x^3 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-3/2} \biggr\} </math>
	<math>~=</math>	<math>~ \biggl[ \frac{\tilde\xi^2}{3}\biggr]^{3/2} \biggl\{ x^3 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-3/2} \biggr\} \, .</math>

By making the substitution, <math>~x \rightarrow \xi/\tilde\xi</math>, this expression becomes identical to the <math>~M_r/M_\mathrm{tot}</math> profile presented just before the "Mass1" subsection, above. In summary, then, we have the following two equally valid expressions for the <math>~M_r</math> profile — one expressed as a function of <math>~\xi</math> and the other expressed as a function of <math>~x</math>:

<math>\frac{M_r(\xi)}{M_\mathrm{tot}}</math>	<math>~=</math>	<math>~ \biggl[\frac{\xi^2}{3}\biggl( 1 + \frac{1}{3}\xi^2 \biggr)^{-1}\biggr]^{3/2} \, ;</math>
<math>\frac{M_r(x)}{M_\mathrm{tot}}</math>	<math>~=</math>	<math>~ \biggl[ \frac{\tilde\xi^2}{3}\biggr]^{3/2} \biggl\{ x^3 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-3/2} \biggr\} \, .</math>

Mean-to-Central Density

From the above line of reasoning we appreciate that, for any spherically symmetric configuration, the ratio of the configuration's mean density to its central density can be obtained by setting the upper limit of our just-completed "Mass2" integration to <math>~x=1</math>. That is to say, quite generally,

<math>~\frac{M_\mathrm{limit}}{M_\mathrm{tot}} </math>	<math>~=</math>	<math>~ \biggl( \frac{\rho_c}{\bar\rho} \biggr)_\mathrm{eq} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr) \int_0^{1} 3x^2 \biggl[ \frac{\rho(x)}{\rho_0} \biggr] dx </math>
<math>~\Rightarrow ~~~ \biggl( \frac{\bar\rho}{\rho_c} \biggr)_\mathrm{eq} </math>	<math>~=</math>	<math>~ \int_0^{1} 3x^2 \biggl[ \frac{\rho(x)}{\rho_0} \biggr] dx </math>

But the integral expression on the righthand side of this relation is also the definition of the structural form factor, <math>~\mathfrak{f}_M</math>, given at the top of this page. Hence, we can say, quite generally, that,

<math>~\mathfrak{f}_M = \frac{\bar\rho}{\rho_c} \, .</math>

And, given that we have just completed this integral for the case of truncated <math>~n=5</math> polytropic structures, we can state, specifically, that,

<math>~\mathfrak{f}_M\biggr|_{n=5} = \biggl[ 1 + \frac{\tilde\xi^2}{3} \biggr]^{-3/2} \, .</math>

Gravitational Potential Energy

As presented at the top of this page, the structural form factor associated with determination of the gravitational potential energy is,

<math>~\mathfrak{f}_W</math>

<math>~\equiv</math>

<math>~ 3\cdot 5 \int_0^1 \biggl\{ \int_0^x \biggl[ \frac{\rho(x)}{\rho_0}\biggr] x^2 dx \biggr\} \biggl[ \frac{\rho(x)}{\rho_0}\biggr] x dx\, .</math>

Given that an expression for the normalized density profile, <math>~\rho(x)/\rho_0</math>, has already been determined, above, we can carry out the nested pair of integrals immediately. Indeed, the integral contained inside of the curly braces has already been completed in the "Mass2" subsection, above, in order to determine the radial mass profile. Specifically, we have already determined that,

<math>~\biggl\{ \int_0^x \biggl[ \frac{\rho(x)}{\rho_0}\biggr] x^2 dx \biggr\} </math>	<math>~=</math>	<math>~\frac{1}{3} \biggl\{ \int_0^{x} 3x^2 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-5/2} dx\biggr\}</math>
	<math>~=</math>	<math>~\frac{1}{3} \biggl\{ x^3 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-3/2} \biggr\} \, .</math>

Hence, with the help of Mathematica's Online Integrator, we have,

<math>~\mathfrak{f}_W</math>	<math>~=</math>	<math>~ 5 \int_0^1 \biggl\{ x^3 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-3/2} \biggr\} \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-5/2} x dx </math>
	<math>~=</math>	<math>~ 5 \int_0^1 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x^2 \biggr]^{-4} x^4 dx </math>
	<math>~=</math>	<math>~ \frac{5}{2^4\cdot 3} \biggl( \frac{\tilde\xi^2}{3}\biggr)^{-5/2} \biggl(1 + \frac{\tilde\xi^2}{3}\biggr)^{-3} \biggl\{ \biggl( \frac{\tilde\xi^2}{3}\biggr)^{1/2} \biggl[ 3\biggl( \frac{\tilde\xi^2}{3}\biggr)^2 - 8\biggl( \frac{\tilde\xi^2}{3}\biggr) - 3 \biggr] + 3\biggl( 1 + \frac{\tilde\xi^2}{3} \biggr)^3\tan^{-1}\biggl[ \biggl( \frac{\tilde\xi^2}{3}\biggr)^{1/2} \biggr] \biggr\} \, . </math>

ASIDE: Now that we have expressions for, both, <math>~\mathfrak{f}_M</math> and <math>~\mathfrak{f}_W</math>, we can determine an analytic expression for the normalized gravitational potential energy for truncated, <math>~n=5</math> polytropes. As is shown in a companion discussion,

<math>~\frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>

<math> - \frac{3}{5} \chi^{-1} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^2 \cdot \frac{\mathfrak{f}_W}{\mathfrak{f}^2_M} \, , </math>

where,

<math>~\equiv</math>

<math> \frac{R_\mathrm{limit}}{R_\mathrm{norm}} = \biggl(\frac{\pi}{2^3\cdot 3^7}\biggr)^{1/2} \tilde\xi \, . </math>

In order to simplify typing, we will switch to the variable,

<math>~\ell \equiv \frac{\tilde\xi}{\sqrt{3}} ~~~\Rightarrow~~~~ \frac{\tilde\xi^2}{3} = \ell^2 \, ,</math>

in which case a summary of derived expressions, from above, gives,

<math>~\chi</math>	<math>~=</math>	<math>~\biggl(\frac{\pi}{2^3\cdot 3^6}\biggr)^{1/2} \ell \, ; </math>
<math>~\mathfrak{f}_M</math>	<math>~=</math>	<math>~( 1 + \ell^2 )^{-3/2} \, ; </math>
<math>~\mathfrak{f}_W</math>	<math>~=</math>	<math>~ \frac{5}{2^4\cdot 3} \cdot \ell^{-5} (1 + \ell^2)^{-3} \biggl\{ \ell [ 3\ell^4 - 8\ell^2 - 3 ] + 3( 1 + \ell^2 )^3\tan^{-1}(\ell ) \biggr\} </math>
	<math>~=</math>	<math>~ \frac{5}{2^4} \cdot \ell^{-5} \biggl[ \ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1 + \ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] \, ; </math>
<math>~\frac{M_\mathrm{limit}}{M_\mathrm{tot} } </math>	<math>~=</math>	<math> \ell^3 (1+\ell^2)^{-3/2} \, . </math>

Hence,

<math>~\biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^{-2} \frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math>~- \frac{3}{5} \biggl(\frac{2^3\cdot 3^6}{\pi}\biggr)^{1/2} \frac{1}{\ell} \cdot (1 + \ell^2)^3 \mathfrak{f}_W </math>
	<math>~=</math>	<math>~- \biggl(\frac{3^8}{2^5 \pi}\biggr)^{1/2} \cdot \ell^{-6} (1 + \ell^2)^3 \biggl[ \ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1 + \ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] </math>
<math>~\Rightarrow ~~~ \frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math>~- \biggl(\frac{3^8}{2^5\pi}\biggr)^{1/2} \cdot \biggl[\ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1+\ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] \, . </math>

This exactly matches the normalized gravitational potential energy derived independently in the context of our exploration of <math>~(n_c, n_e) = (5,1)</math> bipolytropes, referred to in that discussion as <math>~W_\mathrm{core}^*</math>.

Hence, also, as defined in the accompanying introductory discussion, the constant, <math>\mathcal{A}</math>, that appears in our general free-energy equation is (for <math>~n=5</math> polytropic configurations),

<math>~A</math>	<math>~\equiv</math>	<math>\frac{1}{5} \cdot \biggl[ \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr) \frac{1}{\mathfrak{f}_M} \biggr]^2 \cdot \mathfrak{f}_W </math>
	<math>~=</math>	<math>~ \frac{\ell}{2^4} \biggl[ \ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1 + \ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] \, . </math>

Thermal Energy

As presented at the top of this page, the structural form factor associated with determination of the configuration's thermal energy is,

<math>~\mathfrak{f}_A</math>

<math>~\equiv</math>

<math>~ \int_0^1 3\biggl[ \frac{P(x)}{P_0}\biggr] x^2 dx \, ,</math>

Given that an expression for the normalized pressure profile, <math>~P/P_0</math>, has already been provided, above, we can carry out the integral immediately. Specifically, we have,

<math>~\frac{P(\xi)}{P_0} </math>	<math>~=</math>	<math>~\biggl( 1 + \frac{\xi^2}{3} \biggr)^{-3}</math>
<math>~\Rightarrow ~~~~ \frac{P(x)}{P_0} </math>	<math>~=</math>	<math>~\biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x \biggr]^{-3} \, .</math>

Hence, with the aid of Mathematica's Online Integrator, the relevant integral gives,

<math>~\mathfrak{f}_A</math>	<math>~\equiv</math>	<math>~ 3\int_0^1 \biggl[ 1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)x \biggr]^{-3} x^2 dx </math>
	<math>~\equiv</math>	<math>~ \frac{3}{2^3} \biggl\{\biggl(\frac{\tilde\xi^2}{3}\biggr)^{-3/2} \tan^{-1}\biggl[ \biggl(\frac{\tilde\xi^2}{3}\biggr)^{1/2} \biggr] + \biggl(\frac{\tilde\xi^2}{3}\biggr)^{-1}\biggl[1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)\biggr]^{-1} - 2\biggl(\frac{\tilde\xi^2}{3}\biggr)^{-1}\biggl[1 + \biggl(\frac{\tilde\xi^2}{3}\biggr)\biggr]^{-2} \biggr\} \, . </math>

ASIDE: Having this expression for <math>~\mathfrak{f}_A</math> allows us to determine an analytic expression for the coefficient, <math>~\mathcal{B}</math>, that appears in our general expression for the free energy, and that can be straightforwardly used to obtain an expression for the thermal energy content of <math>~n=5 (\gamma=6/5)</math> polytropic configurations. From our accompanying introductory discussion, we have,

<math>~\mathcal{B}</math>

<math>~\equiv</math>

<math> \biggl(\frac{3}{2^2 \pi} \biggr)^{1/5} \biggl[ \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}}\biggr) \frac{1}{\mathfrak{f}_M} \biggr]_\mathrm{eq}^{6/5} \cdot \mathfrak{f}_A \, . </math>

If, as above, we adopt the simplifying variable notation,

<math>~\ell \equiv \frac{\tilde\xi}{\sqrt{3}} ~~~\Rightarrow~~~~ \frac{\tilde\xi^2}{3} = \ell^2 \, ,</math>

the various factors in the definition of <math>~\mathcal{B}</math> and <math>~S_\mathrm{therm}</math> are (see above),

<math>~\chi</math>	<math>~=</math>	<math>~\biggl(\frac{\pi}{2^3\cdot 3^6}\biggr)^{1/2} \ell \, ; </math>
<math>~\biggl(\frac{M_\mathrm{limit}}{M_\mathrm{tot} }\biggr)\frac{1}{\mathfrak{f}_M} </math>	<math>~=</math>	<math> \ell^3 \, ; </math>
<math>~\mathfrak{f}_A</math>	<math>~=</math>	<math>~ \frac{3}{2^3} [ \ell^{-3} \tan^{-1}(\ell ) + \ell^{-2}(1+\ell^2)^{-1} - 2\ell^{-2}(1+\ell^2)^{-2} ] \, . </math>
	<math>~=</math>	<math>~ \frac{3}{2^3} \ell^{-3} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] \, . </math>

Hence,

<math>~\mathcal{B}</math>

<math> \biggl(\frac{3^6}{2^{17} \pi} \biggr)^{1/5}~\ell^{3/5} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] \, ; </math>

and (see here and here),

<math>~\frac{S_\mathrm{therm}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math> \frac{3}{2}(\gamma - 1)\biggl[ \frac{\mathfrak{S}_\mathrm{therm}}{E_\mathrm{norm}}\biggr] = \frac{3}{2} \cdot \chi^{3(1-\gamma)} \mathcal{B} = \frac{3}{2} \cdot \chi^{-3/5} \mathcal{B} </math>
	<math>~=</math>	<math> \frac{3}{2} \cdot \biggl[ \biggl(\frac{\pi}{2^3\cdot 3^6}\biggr)^{1/2} \ell \biggr]^{-3/5} \biggl(\frac{3^6}{2^{17} \pi} \biggr)^{1/5} \ell^{3/5} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] </math>
	<math>~=</math>	<math> \biggl[ \frac{3^{10}}{2^{10}} \biggl(\frac{2^9\cdot 3^{18}}{\pi^3}\biggr) \biggl(\frac{3^{12}}{2^{34} \pi^2} \biggr) \biggr]^{1/10} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] </math>
	<math>~=</math>	<math> \biggl(\frac{3^{8}}{2^{7}\pi}\biggr)^{1/2} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] \, . </math>

This exactly matches the normalized thermal energy derived independently in the context of our exploration of <math>~(n_c, n_e) = (5,1)</math> bipolytropes, referred to in that discussion as <math>~S_\mathrm{core}^*</math>. Its similarity to the expression for the gravitational potential energy — which is relevant to the virial theorem — is more apparent if it is rewritten in the following form:

<math>~\frac{S_\mathrm{therm}}{E_\mathrm{norm}}</math>

<math>\frac{1}{2} \biggl(\frac{3^{8}}{2^{5}\pi}\biggr)^{1/2} [ \ell (\ell^4-1) (1+\ell^2)^{-3} + \tan^{-1}(\ell )] \, . </math>

Summary (n=5)

In summary, for <math>~n=5</math> structures we have,

Structural Form Factors (n = 5)

<math>~\mathfrak{f}_M</math>	<math>~=</math>	<math>~ ( 1 + \ell^2 )^{-3/2} </math>
<math>~\mathfrak{f}_W</math>	<math>~=</math>	<math>~ \frac{5}{2^4} \cdot \ell^{-5} \biggl[ \ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1 + \ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] </math>
<math>~\mathfrak{f}_A</math>	<math>~=</math>	<math>~ \frac{3}{2^3} \ell^{-3} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] </math>

Free-Energy Coefficients (n = 5)

<math>~\mathcal{A}</math>	<math>~=</math>	<math>~ \frac{\ell}{2^4} \biggl[ \ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1 + \ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] </math>
<math>~\mathcal{B}</math>	<math>~=</math>	<math> \biggl(\frac{3^6}{2^{17} \pi} \biggr)^{1/5}~\ell^{3/5} [ \tan^{-1}(\ell ) + \ell (\ell^2-1) (1+\ell^2)^{-2} ] </math>

Normalized Energies (n = 5)

<math>~\frac{S_\mathrm{therm}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math>~ \frac{1}{2} \biggl(\frac{3^{8}}{2^{5}\pi}\biggr)^{1/2} [ \ell (\ell^4-1) (1+\ell^2)^{-3} + \tan^{-1}(\ell )] </math>
<math>~\frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math>~ - \biggl(\frac{3^8}{2^5\pi}\biggr)^{1/2} \cdot \biggl[\ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1+\ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] </math>

Reality Check (n=5)

<math>~2\biggl(\frac{S_\mathrm{therm}}{E_\mathrm{norm}}\biggr)+ \frac{W_\mathrm{grav}}{E_\mathrm{norm}}</math>	<math>~=</math>	<math>~\biggl(\frac{3^{8}}{2^{5}\pi}\biggr)^{1/2}\biggl\{ [ \ell (\ell^4-1) (1+\ell^2)^{-3} + \tan^{-1}(\ell )] - \biggl[\ell \biggl( \ell^4 - \frac{8}{3}\ell^2 - 1 \biggr)(1+\ell^2)^{-3} + \tan^{-1}(\ell ) \biggr] \biggr\} </math>
	<math>~=</math>	<math>~\biggl(\frac{3^{8}}{2^{5}\pi}\biggr)^{1/2} \biggl[\frac{8}{3}\ell^3 (1+\ell^2)^{-3}\biggr] </math>
	<math>~=</math>	<math>~\biggl(\frac{2 \cdot 3^{6}}{\pi}\biggr)^{1/2} \biggl[\frac{\ell}{ (1+\ell^2)} \biggr]^3 \, . </math>

For embedded polytropes, this should be compared against the expectation (prediction) provided by Stahler's equilibrium models, as detailed above. Given that, for <math>~n=5</math> polytropes — see the "Mass1" discussion above and our accompanying tabular summary of relevant properties,

<math> ~\frac{M_\mathrm{limit}}{M_\mathrm{tot}} = \biggl[ \ell^2(1+\ell^2)^{-1} \biggr]^{3/2} </math>

;

<math> ~\theta_5 = ( 1 + \ell^2 )^{-1/2} </math>

and

<math> ~-\frac{d\theta_5}{d\xi} \biggr|_{\xi_e} = 3^{1/2} \ell ( 1 + \ell^2 )^{-3/2} \, , </math>

the expectation is that,

<math>~\frac{4\pi P_e R_\mathrm{eq}^3}{E_\mathrm{norm}} </math>	<math>~=</math>	<math>~ \biggl[ \frac{(n+1)^3}{4\pi}\biggr]^{1/(n-3)} \biggl[ \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)\frac{1}{(-\theta'_n)_{\tilde\xi}}\biggr]^{(n-5)/(n-3)} (\theta_n)_{\tilde\xi}^{(n+1)} \tilde\xi^{(n+1)/(n-3)} </math>
	<math>~=</math>	<math>~ \biggl[ \frac{2\cdot 3^3}{\pi}\biggr]^{1/2} ( 1 + \ell^2 )^{-3} (3^{1/2}\ell)^{3} </math>
	<math>~=</math>	<math>~ \biggl( \frac{2\cdot 3^6}{\pi}\biggr)^{1/2} \biggl[ \frac{\ell}{( 1 + \ell^2 )} \biggr]^{3} \, . </math>

This precisely matches our sum of the thermal and gravitational potential energies, as just determined using our expressions for the structural form factors. This gives us confidence that our form-factor expressions are correct, at least in the case of embedded <math>~n=5</math> polytropic structures.