User:Tohline/SSC/Structure/Polytropes/VirialSummary

Virial Equilibrium of Pressure-Truncated Polytropes

Here we will draw heavily from …

• An accompanying Free Energy Synopsis;
• A detailed analysis of the Virial Equilibrium of Adiabatic Spheres.

Groundwork

Basic Relation

In the context of spherically symmetric, pressure-truncated polytropic configurations, the relevant free-energy expression is,

<math>~\mathfrak{G}</math>	<math>~=</math>	<math>~W_\mathrm{grav} + U_\mathrm{int} + P_eV</math>
	<math>~=</math>	<math>~ - 3\mathcal{A} \biggl[\frac{GM^2}{R} \biggr] + n\mathcal{B} \biggl[ \frac{K_nM^{(n+1)/n}}{R^{3/n}} \biggr] + \frac{4\pi}{3} \cdot P_e R^3 \, ,</math>

where, when written in terms of the trio of structural form factors, <math>~\tilde{\mathfrak{f}}_M,</math> <math>~\tilde{\mathfrak{f}}_M,</math> and <math>~\tilde{\mathfrak{f}}_M,</math> the pair of constants,

<math>~\mathcal{A} \equiv \frac{1}{5} \cdot \frac{\tilde{\mathfrak{f}}_W}{\tilde{\mathfrak{f}}_M^2}</math>

and

<math>\mathcal{B} \equiv \biggl(\frac{4\pi}{3} \biggr)^{-1/n} \frac{\tilde{\mathfrak{f}}_A}{\tilde{\mathfrak{f}}_M^{(n+1)/n}} \, .</math>

Often-Referenced Dimensionless Expressions

When rewritten in a suitably dimensionless form — see two useful alternatives, below — this expression becomes,

<math>~\mathfrak{G}^*</math>

<math>~=</math>

<math>~- a x^{-1} + bx^{-3/n} + c x^3 \, ,</math>

where <math>~x</math> is the configuration's dimensionless radius and <math>~a</math>, <math>~b</math>, and <math>~c</math> are constants. We therefore have,

<math>~\frac{d\mathfrak{G}^*}{dx}</math>

<math>~=</math>

<math>~\frac{1}{x^2} \biggl[ a - \biggl( \frac{3b}{n} \biggr) x^{(n-3)/n} + 3c x^4 \biggr] \, ,</math>

and,

<math>~\frac{d^2\mathfrak{G}^*}{dx^2}</math>

<math>~=</math>

<math>~\frac{1}{x^3} \biggl[\biggl(\frac{n+3}{n}\biggr) \biggl( \frac{3b}{n} \biggr) x^{(n-3)/n} + 6c x^4 - 2a \biggr] \, .</math>

Virial equilibrium is obtained when <math>~d\mathfrak{G}^*/dx = 0</math>, that is, when

<math>~\biggl( \frac{3b}{n} \biggr) x_\mathrm{eq}^{(n-3)/n} </math>

<math>~=</math>

<math>~ a + 3c x_\mathrm{eq}^4 \, .</math>

And along an equilibrium sequence, the specific equilibrium state that marks a transition from dynamically stable to dynamically unstable configurations — henceforth labeled as having the critical radius, <math>~x_\mathrm{crit}</math> — is identified by setting <math>~d^2\mathfrak{G}^*/dx^2 = 0</math>, that is, it is the configuration for which,

<math>~0</math>	<math>~=</math>	<math>~\biggl[\biggl(\frac{n+3}{n}\biggr) \biggl( \frac{3b}{n} \biggr) x^{(n-3)/n} + 6c x^4 - 2a \biggr]_{x = x_\mathrm{eq}}</math>
<math>~\Rightarrow ~~~ x_\mathrm{crit}^4 </math>	<math>~=</math>	<math>~ \frac{a}{3^2c}\biggl(\frac{n - 3}{n+1}\biggr) \, . </math>

Inserting the adiabatic exponent in place of the polytropic index via the relation, <math>~n = (\gamma - 1)^{-1}</math>, we have equivalently,

<math>~ x_\mathrm{crit}^4 </math>

<math>~=</math>

<math>~ \frac{a}{3^2c}\biggl(\frac{4-3\gamma}{\gamma}\biggr) \, . </math>

Useful Recognition

By comparing various terms in the first two algebraic Setup expressions, above, It is clear that,

<math>~W^*_\mathrm{grav} = -ax^{-1}</math>

and,

<math>~U^*_\mathrm{int} = bx^{-3/n} \, .</math>

Notice, then, that in every equilibrium configuration, we should find,

<math>~- \frac{U^*_\mathrm{int}}{W^*_\mathrm{grav}}\biggr|_\mathrm{eq}</math>	<math>~=</math>	<math>~ \biggl(\frac{b}{a}\biggr) x_\mathrm{eq}^{(n-3)/n} = \frac{n}{3a} \biggl[ a + 3cx^4_\mathrm{eq} \biggr] </math>
	<math>~=</math>	<math>~ \frac{n}{3} \biggl[ 1 + \biggl(\frac{3c}{a}\biggr) x^4_\mathrm{eq} \biggr] \, . </math>

And, specifically in the critical configuration we should find that,

<math>~- \frac{U^*_\mathrm{int}}{W^*_\mathrm{grav}}\biggr|_\mathrm{crit}</math>	<math>~=</math>	<math>~ \frac{1}{3(\gamma-1)} \biggl[ 1 + \frac{1}{3}\biggl(\frac{4-3\gamma}{\gamma}\biggr) \biggr] = \frac{4}{3^2\gamma(\gamma-1)} </math>
<math>~\Rightarrow ~~~\frac{S^*_\mathrm{therm}}{W^*_\mathrm{grav}}\biggr|_\mathrm{crit}</math>	<math>~=</math>	<math>~ -\frac{2}{3\gamma} \, . </math>

The equivalent of this last expression also appears at the end of subsection ⑦ of an accompanying Tabular Overview.

Equilibrium Sequences

In all of the polytropic configurations being considered here, <math>~K_\mathrm{n}</math> is a constant — that is, the specific entropy of all fluid elements is assumed to be the same, both spatially and temporally.

Fix Mass While Varying External Pressure

In this case, we want to examine undulations of a two-dimensional free-energy surface that results from allowing <math>~R</math> and <math>~P_e</math> to vary while holding <math>~M</math> fixed. In our accompanying, more detailed discussion, this is referred to as Case M. Adopting the normalizations,

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

<math>~\equiv</math>

<math>~ \biggl[ \biggl( \frac{G}{K_n} \biggr)^n M^{n-1} \biggr]^{1/(n-3)} \, , </math>

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

<math>~\equiv</math>

<math>~ \biggl[ \frac{K_n^{4n}}{G^{3(n+1)} M^{2(n+1)}} \biggr]^{1/(n-3)} </math>

and,

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

<math>~\equiv</math>

<math>~ P_\mathrm{norm} R^3_\mathrm{norm} \, , </math>

— which, as is detailed in an accompanying discussion, are similar but not identical to the normalizations adopted by Horedt (1970) and by Whitworth (1981) — the coefficients in the above-presented Basic Relations become,

<math>~a</math>

<math>~\equiv</math>

<math>~3\mathcal{A} \, , </math>

<math>~b</math>

<math>~\equiv</math>

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

and,

<math>~c</math>

<math>~\equiv</math>

<math>~\frac{4\pi}{3}\biggl( \frac{P_e}{P_\mathrm{norm}} \biggr) \, . </math>

The relevant dimensionless free-energy surface is, then, given by the expression,

Case M Free-Energy Surface
<math>~\mathfrak{G}_{K,M}^* \equiv \frac{\mathfrak{G}_{K,M}}{E_\mathrm{norm}} </math> <math>~=</math> <math>~ -3\mathcal{A} \biggl(\frac{R}{R_\mathrm{norm}}\biggr)^{-1} +~ n\mathcal{B} \biggl(\frac{R}{R_\mathrm{norm}}\biggr)^{-3/n} +~ \biggl( \frac{4\pi}{3} \biggr) \frac{P_e}{P_\mathrm{norm}} \biggl(\frac{R}{R_\mathrm{norm}}\biggr)^3 \, . </math>

Fix External Pressure While Varying Mass

In this case, we want to examine undulations of a two-dimensional free-energy surface that results from allowing <math>~R</math> and <math>~M</math> to vary while holding <math>~P_e</math> fixed. In our accompanying, more detailed discussion, this is referred to as Case P. Motivated by Stahler's (1983) work, here we adopt the normalizations,

<math>~R_\mathrm{SWS}</math>	<math>~\equiv</math>	<math>~\biggl( \frac{n+1}{nG} \biggr)^{1/2} K_n^{n/(n+1)} P_\mathrm{e}^{(1-n)/[2(n+1)]} \, ,</math>		<math>~M_\mathrm{SWS}</math>	<math>~\equiv</math>	<math>~\biggl( \frac{n+1}{nG} \biggr)^{3/2} K_n^{2n/(n+1)} P_\mathrm{e}^{(3-n)/[2(n+1)]} </math>	and,
<math>~E_\mathrm{SWS}</math>	<math>~\equiv</math>	<math>~ \biggl( \frac{n}{n+1} \biggr) \frac{GM_\mathrm{SWS}^2}{R_\mathrm{SWS}} = \biggl( \frac{n+1}{n} \biggr)^{3/2} G^{-3/2}K_n^{3n/(n+1)} P_\mathrm{e}^{(5-n)/[2(n+1)]} \, .</math>

the coefficients in the above-presented Basic Relations become,

<math>~a</math>

<math>~\equiv</math>

<math>~3 \mathcal{A} \biggl( \frac{n+1}{n} \biggr)\biggl( \frac{M}{M_\mathrm{SWS}}\biggr)^2 \, , </math>

<math>~b</math>

<math>~\equiv</math>

<math>~n\mathcal{B} \biggl(\frac{M}{M_\mathrm{SWS}}\biggr)^{(n+1)/n} </math>

and,

<math>~c</math>

<math>~\equiv</math>

<math>~\frac{4\pi}{3} \, , </math>

where the pair of constants, <math>~\mathcal{A}</math> and <math>~\mathcal{B}</math>, have the same definitions in terms of the structural form factors as provided above. The relevant dimensionless free-energy surface is, then, given by the expression,

Case P:   Free-Energy Surfaces

<math>~\mathfrak{G}_{K,P_e}^* \equiv \frac{\mathfrak{G}_{K,P_e}}{E_\mathrm{SWS}}</math> <math>~=</math> <math>~- 3 \mathcal{A} \biggl( \frac{n+1}{n} \biggr)\biggl( \frac{M}{M_\mathrm{SWS}}\biggr)^2 \biggl(\frac{R}{R_\mathrm{SWS}}\biggr)^{-1} + n\mathcal{B} \biggl(\frac{M}{M_\mathrm{SWS}}\biggr)^{(n+1)/n} \biggl(\frac{R}{R_\mathrm{SWS}}\biggr)^{-3/n} + \frac{4\pi}{3} \biggl( \frac{R}{R_\mathrm{SWS}}\biggr)^3 \, . </math>

Across this Case P free-energy surface, extrema — and, hence, equilibrium configurations — will arise wherever the virial-equilibrium condition is met, that is, wherever

Case P:   Virial Equilibrium Sequences
<math>~0</math> <math>~=</math> <math>~ \biggl( \frac{R}{R_\mathrm{SWS}}\biggr)^4 -\frac{3\mathcal{B}}{4\pi} \biggl(\frac{M}{M_\mathrm{SWS}}\biggr)^{(n+1)/n} \biggl( \frac{R}{R_\mathrm{SWS}}\biggr)^{(n-3)/n} + \frac{3 \mathcal{A}}{4\pi} \biggl( \frac{n+1}{n} \biggr)\biggl( \frac{M}{M_\mathrm{SWS}}\biggr)^2 \, .</math>

An equilibrium model sequence is thereby defined for each chosen polytropic index in the range, <math>~0 \le n < \infty</math>.

Along each equilibrium sequence for which <math>~3 \le n < \infty</math>, there is one specific equilibrium state that marks a transition from dynamically stable to dynamically unstable configurations. For a given mass, the radius of this critical configuration is identified by the relation,

<math>~ \biggl( \frac{R_\mathrm{eq}}{R_\mathrm{SWS}}\biggr)_\mathrm{crit}^4 </math>

<math>~=</math>

<math>~ \frac{\mathcal{A}}{4\pi}\biggl(\frac{n - 3}{n}\biggr) \biggl( \frac{M}{M_\mathrm{SWS}}\biggr)^2 \, . </math>

---

Below, we will examine the behavior of individual virial-equilibrium sequences, using various physical arguments to justify our choice of specific expressions for the coefficients, <math>~\mathcal{A}</math> and <math>~\mathcal{B}</math>. Here, in an effort to provide a broad overview, we set all three structural form factors to unity, in which case the pair of coefficients,

<math>~\mathcal{A} = \frac{1}{5}</math>       and       <math>~\mathcal{B} = \biggl( \frac{3}{4\pi} \biggr)^{1/n}</math>,

and the resulting mass-radius relation of equilibrium sequences is governed by the algebraic mass-radius relation,

<math>~0</math>

<math>~=</math>

<math>~ \biggl( \frac{R}{R_\mathrm{SWS}}\biggr)^4 - \biggl( \frac{R}{R_\mathrm{SWS}}\biggr)^{(n-3)/n}\biggl[ \biggl(\frac{3}{4\pi} \biggr) \frac{M}{M_\mathrm{SWS}}\biggr]^{(n+1)/n} + ~\frac{3}{20\pi} \biggl( \frac{n+1}{n}\biggr) \biggl( \frac{M}{M_\mathrm{SWS}}\biggr)^2 \, .</math>

The left-hand panel of Figure 1 displays this behavior for equilibrium sequences having seven different values of the polytropic index, as labeled. As has been demonstrated in an accompanying discussion, this governing mass-radius relation can be analytically manipulated into a form that provides either an explicit <math>~M(R)</math> or <math>~R(M)</math> relation for the cases labeled, <math>~n = 1, 3,</math> and <math>~\infty</math>; a generic root-finding technique has been used to generate points along each of the other depicted equilibrium sequences.

Figure 1:   Virial-Analysis-Based Equilibrium Sequences

For comparison, the schematic diagram displayed on the righthand side of the figure is a reproduction of Figure 17 from Appendix B of Stahler (1983). It seems that our derived, analytically prescribable, mass-radius relationship — which is, in essence, a statement of the scalar virial theorem — embodies most of the attributes of the mass-radius relationship for pressure-truncated polytropes that were already understood, and conveyed schematically, by Stahler in 1983.

See Also

• Index to a Variety of Free-Energy and/or Virial Analyses

© 2014 - 2021 by Joel E. Tohline |   H_Book Home   |   YouTube   | Appendices: | Equations | Variables | References | Ramblings | Images | myphys.lsu | ADS | Recommended citation:   Tohline, Joel E. (2021), The Structure, Stability, & Dynamics of Self-Gravitating Fluids, a (MediaWiki-based) Vistrails.org publication, https://www.vistrails.org/index.php/User:Tohline/citation