User:Tohline/SSC/Virial/PolytropesEmbeddedOutline

Virial Equilibrium of Embedded Polytropic Spheres

Click here for technical discussion of this Free-Energy surface

Overview

The free-energy function that is relevant to a discussion of the structure and stability of a pressure-truncated configuration having polytropic index, <math>~n</math>, has the form,

<math>~\mathcal{G}(x)</math>

<math>~=</math>

<math> -ax^{-1} +b x^{-3/n} + c x^3 \, , </math>

where <math>~x</math> identifies the size of the configuration. (As is explained more fully, below, the above figure displays a free-energy surface of this form for the case, <math>~n=5</math>.) If the coefficients, <math>~a, b</math>, and <math>~c</math>, are held constant while varying the configuration's size, we see that,

<math>~\frac{d\mathcal{G}}{dx}</math>	<math>~=</math>	<math> ax^{-2} - \frac{3b}{n}\cdot x^{-(3+n)/n} + 3c x^2 </math>
	<math>~=</math>	<math> x^{-2} \biggl[ a - \frac{3b}{n}\cdot x^{(n-3)/n} + 3c x^4 \biggr] \, , </math>

and,

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

<math>~=</math>

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

Equilibrium Configurations

The size, <math>~x_\mathrm{eq}</math>, of each equilibrium configuration is determined by setting, <math>d\mathcal{G}/dx = 0</math>. Hence, <math>~x_\mathrm{eq}</math> is given by the root(s) of the polynomial expression,

<math>~x^{(n-3)/n}_\mathrm{eq} </math>

<math>~=</math>

<math>\frac{n}{b} \biggl[ \frac{a}{3} + c\cdot x^4_\mathrm{eq} \biggr] \, . </math>

(The equilibrium radii of <math>~n = 5</math> polytropic configurations having a variety of different masses are identified by the sequence of a dozen, small colored spherical dots in the above figure.)

Stability

The relative stability of each equilibrium configuration is determined by the sign of the second derivative of the free-energy function, evaluated at the specified equilibrium radius. Specifically, the systems being considered here are stable if the second derivative is positive, but they are unstable if the second derivative is negative. Evaluating the second derivative in this manner gives,

<math>~\biggl[ x^{3} \cdot \frac{d^2\mathcal{G}}{dx^2}\biggr]_\mathrm{eq}</math>	<math>~=</math>	<math> -2a + \frac{3(3+n)b}{n^2} \biggl[ \frac{na}{3b} + \frac{nc}{b}\cdot x^4_\mathrm{eq} \biggr] + 6c x^4_\mathrm{eq} </math>
	<math>~=</math>	<math> -2a + \frac{(3+n)a}{n} + \frac{3(3+n)c}{n} \cdot x^4_\mathrm{eq} + 6c x^4_\mathrm{eq} </math>
	<math>~=</math>	<math>\frac{9(n+1)c}{n}\cdot x^4_\mathrm{eq} - \frac{a(n-3)}{n} \, . </math>

Defining <math>~x_\mathrm{crit}</math> as the equilibrium radius at which this function goes to zero gives,

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

<math>~\equiv</math>

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

(The small red spherical dot in the above figure identifies the equilibrium configuration at <math>~x_\mathrm{crit} </math>.) We conclude, therefore, that pressure-truncated, equilibrium polytropic configurations having <math>~n > 3</math> are stable if,

<math>~x_\mathrm{eq}</math>

<math>~></math>

<math> ~x_\mathrm{crit} \, , </math>

while they are unstable if,

<math>~x_\mathrm{eq}</math>

<math>~<</math>

<math> ~x_\mathrm{crit} \, . </math>

The Physics

The following discussion will focus on sequences of equilibrium configurations that have a polytropic index <math>~n > 3</math> because, as has been foreshadowed in the above overview, such sequences include both stable and unstable equilbria and are therefore more interesting in an astrophysical context. Isothermal sequences — corresponding to <math>~n = \infty</math> — are of particular astrophysical interest; however, we will devote a great deal of attention to <math>~n=5</math> configurations because their structures can be defined entirely in terms of analytic expressions.

In order to determine the equilibrium radius, <math>~R_\mathrm{eq}</math>, of any pressure-truncated polytropic configuration, we must specify the configuration's mass, <math>~M_\mathrm{limit}</math>, its polytropic constant, <math>~K</math>, and the pressure, <math>~P_e</math>, of the external medium in which the configuration is embedded, and locate extrema in the resulting <math>~\mathfrak{G}(R)</math> function. Then, a sequence of equilibria can be identified if, for example:

• Case P: <math>~P_e</math> is varied while holding <math>~K</math> and <math>~M_\mathrm{limit}</math> fixed; or
• Case M: <math>~M_\mathrm{limit}</math> is varied while holding <math>~K</math> and <math>~P_e</math> fixed.

In the first case, the analysis reveals how <math>~R_\mathrm{eq}</math> varies with the applied external pressure and usually is displayed as a <math>~P_e(R_\mathrm{eq})</math> function. The second case identifies a mass-radius relationship for the polytropic sequence under consideration and is usually displayed as a <math>~M_\mathrm{limit}(R_\mathrm{eq})</math> function. (In the figure at the top of this page, a "Case M" mass-radius relation for pressure-truncated, <math>~n = 5</math> polytropic configurations is traced by the sequence of a dozen, small colored spherical dots that each reside at an extremum in the displayed free-energy function.)

Our Case P Analysis (raw)

As has been both summarized and detailed in an accompanying discussion, our Case P analysis has demonstrated that the following,

Algebraic Free-Energy Function

<math> \mathfrak{G}^* = -3\mathcal{A} \chi^{-1} +~ n\mathcal{B} \chi^{-3/n} +~ \mathcal{D}\chi^3 \, , </math>

properly governs the equilibrium structure and stability of pressure-truncated polytropic configurations. This expression is identical to the free-energy function given above if the following coefficient and variable substitutions are made:

Our Case P Analysis

<math>~a</math> <math>~\rightarrow</math> <math>~3\mathcal{A}</math> <math>~b</math> <math>~\rightarrow</math> <math>~n\mathcal{B} </math> <math>~c</math> <math>~\rightarrow</math> <math>~\mathcal{D} \equiv \frac{4\pi}{3} \biggl(\frac{P_e}{P_\mathrm{norm}}\biggr)</math> <math>~x</math> <math>~\rightarrow</math> <math>~\chi \equiv \frac{R}{R_\mathrm{norm}}</math> <math>~\mathcal{G}</math> <math>~\rightarrow</math> <math>~\mathfrak{G}^{*} \equiv \frac{\mathfrak{G}}{E_\mathrm{norm}}</math>

where — see, for example, our accompanying review,

<math>~R_\mathrm{norm}</math>	<math>~=</math>	<math>~\biggl[ \biggl( \frac{G}{K} \biggr)^n M_\mathrm{tot}^{n-1} \biggr]^{1/(n-3)} \, ,</math>
<math>~P_\mathrm{norm}</math>	<math>~=</math>	<math>~\biggl[ \frac{K^{4n}}{G^{3(n+1)} M_\mathrm{tot}^{2(n+1)}} \biggr]^{1/(n-3)} \, , </math>
<math>~E_\mathrm{norm}</math>	<math>~=</math>	<math>~ \biggl[ K^n G^{-3}M_\mathrm{tot}^{n-5} \biggr]^{1/(n-3)} \, ,</math>

and, in terms of the structural form factors, <math>~\tilde\mathfrak{f}_M</math>, <math>~\tilde\mathfrak{f}_A</math>, and <math>~\tilde\mathfrak{f}_W</math>,

<math>~\mathcal{A}</math>	<math>~=</math>	<math>\frac{1}{5} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}} \biggr)^2 \cdot \frac{\tilde\mathfrak{f}_W}{\tilde\mathfrak{f}_M^2} \, , </math>
<math>~\mathcal{B}</math>	<math>~=</math>	<math> \biggl(\frac{3}{4\pi}\biggr)^{1/n} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}}\biggr)^{(n+1)/n} \frac{\tilde\mathfrak{f}_A}{\tilde\mathfrak{f}_M^{(n+1)/n}} \, . </math>

Our Case P Analysis (compact)

As has been both summarized and detailed in an accompanying discussion, our Case P analysis has demonstrated that the following,

Renormalized Free-Energy Function

<math> \mathfrak{G}^{**} \equiv \mathfrak{G}^* \biggl[ \frac{\mathcal{A}^3}{\mathcal{B}^n} \biggr]^{1/(n-3)} = -3 \Chi^{-1} +~ n\Chi^{-3/n} +~ \Pi_\mathrm{ad}\Chi^3 \, , </math>

properly governs the equilibrium structure and stability of pressure-truncated polytropic configurations. This expression is identical to the free-energy function given above if the following coefficient and variable substitutions are made:

Our Case P Analysis

<math>~a</math> <math>~\rightarrow</math> <math>~3</math> <math>~b</math> <math>~\rightarrow</math> <math>~n</math> <math>~c</math> <math>~\rightarrow</math> <math>~\Pi_\mathrm{ad} \equiv \frac{P_e}{P_\mathrm{ad}}</math> <math>~x</math> <math>~\rightarrow</math> <math>~\Chi \equiv \frac{R}{R_\mathrm{ad}}</math> <math>~\mathcal{G}</math> <math>~\rightarrow</math> <math>~\mathfrak{G}^{**} </math>

where,

Whitworth's (1981) Case P Analysis

Whitworth's (1981) related Case P analysis of pressure-truncated polytropic spheres produces the following governing free-energy function — referred to by Whitworth as the "global potential function":

<math> \frac{2\mathcal{U}}{3M_0 K_1} = -\frac{3}{2} \biggl( \frac{R}{R_\mathrm{rf}}\biggr)^{-1} +~ \frac{2n}{3}\biggl( \frac{R}{R_\mathrm{rf}}\biggr)^{-3/n} +~ \frac{1}{6}\biggl(\frac{P_e}{P_\mathrm{rf}}\biggr) \biggl( \frac{R}{R_\mathrm{rf}}\biggr)^3 \, ; </math>

this expression is obtained from Whitworth's equation (10) after setting <math>~\delta_{1\eta} = 0</math>, that is, by choosing to ignore isothermal systems, and after setting <math>~\eta = (n+1)/n</math>, that is, after rewriting his adiabatic exponent <math>~(\eta)</math> in terms of the corresponding polytropic index. Whitworth's expression also is identical to the free-energy function given above if the following coefficient and variable substitutions are made:

Whitworth's (1981) Case P Analysis

<math>~a</math> <math>~\rightarrow</math> <math>~\frac{3}{2}</math> <math>~b</math> <math>~\rightarrow</math> <math>~\frac{2n}{3}</math> <math>~c</math> <math>~\rightarrow</math> <math>~\frac{1}{6}\biggl(\frac{P_e}{P_\mathrm{rf}}\biggr)</math> <math>~x</math> <math>~\rightarrow</math> <math>~\frac{R}{R_\mathrm{rf}}</math> <math>~\mathcal{G}</math> <math>~\rightarrow</math> <math>~\frac{2}{3} \biggl( \frac{\mathcal{U}}{U_\mathrm{norm}} \biggr) </math>

where (see an accompanying ASIDE),

<math>~R_\mathrm{rf}</math>	<math>~\equiv</math>	<math> \biggl[ \frac{\pi}{5^n} \biggl( \frac{2^2}{3}\biggr)^{(n+1)} K^{-n} G^{n} M_\mathrm{limit}^{n-1} \biggr]^{1/(n-3)} </math>
	<math>~=</math>	<math>~R_\mathrm{norm} \biggl[ \frac{\pi}{5^n} \biggl( \frac{2^2}{3}\biggr)^{(n+1)} \biggr]^{1/(n-3)} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}}\biggr)^{(n-1)/(n-3)} \, , </math>
<math>~P_\mathrm{rf}</math>	<math>~\equiv</math>	<math>~\biggl[ 2^{-2(5n+1)}\biggl( \frac{3^4\cdot 5^3}{\pi} \biggr)^{n+1} K^{4n} G^{-3(n+1)} M_\mathrm{limit}^{-2(n+1)}\biggr]^{1/(n-3)} </math>
	<math>~=</math>	<math>~P_\mathrm{norm} \biggl[ 2^{-2(5n+1)}\biggl( \frac{3^4\cdot 5^3}{\pi} \biggr)^{n+1} \biggr]^{1/(n-3)} \, , </math>
<math>~U_\mathrm{norm} \equiv (M_0K_1)_\mathrm{Whitworth}</math>	<math>~=</math>	<math>~\biggl[ \biggl( \frac{3^4\cdot 5^3}{2^8\pi} \biggr) K^n G^{-3} M_\mathrm{limit}^{n-5}\biggr]^{1/(n-3)} </math>
	<math>~=</math>	<math>~E_\mathrm{norm} \biggl( \frac{3^4\cdot 5^3}{2^8\pi} \biggr)^{1/(n-3)} \biggl( \frac{M_\mathrm{limit}}{M_\mathrm{tot}}\biggr)^{(n-5)/(n-3)} \, . </math>

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Outline of Detailed Investigations Leading to Above Summary

First Effort

My first attempt to analytically define the free energy, and then the virial equilibrium, of pressure-truncated (embedded) polytropic spheres was developed as a direct extension of my description of the virial equilibrium of isolated polytropes. An important outcome of this "first effort" was the unveiling of analytic expressions for the key structural form factors, both for isolated polytropes and, separately, for pressure-truncated polytropic structures.

I am very confident that the form-factor expressions presented for isolated polytropes are all correct because they have been cross-checked with expressions for closely related "integral" parameters discussed by Chandrasekhar [C67]. Although the form-factor expressions derived for pressure-truncated polytropes make some sense — they look very similar to the ones presented for isolated polytropes and seem to behave properly for models which, based on detailed force-balanced analysis, are known to be in equilibrium — I have much less confidence that they are correct. A couple of strategies were developed in an effort to demonstrate the validity and utility of these more general form-factor expressions, resulting in the derivation of a concise virial equilibrium relation,

<math>\Pi_\mathrm{ad} = \chi_\mathrm{ad}^{-3\gamma} - \chi_\mathrm{ad}^{-4} \, ,</math>

that incorporates the newly defined normalization parameters, <math>~R_\mathrm{ad}</math> and <math>~P_\mathrm{ad}</math>. But subsequent derivations aimed at more conclusively demonstrating the correctness of the more general form-factor expressions were messy and got bogged down.

Second Effort

My second attempt to analytically define the free energy, and then the virial equilibrium, of pressure-truncated (embedded) polytropic spheres built upon my first effort and, for a couple of different polytropic indexes, focused on comparing the mass-radius relationship embodied in detailed force-balanced models against the mass-radius relationship implied by the virial theorem. A lot of reasonable results seem to have arisen from a discussion of models (done numerically using Excel) with <math>~n=4</math> polytropic index. And there are some nice aspects of models with an <math>~n=5</math> index, but these models raise some serious concerns related to the fact that two of our "derived" form-factor expressions involve division by the factor, <math>~(5-n)</math>, that is, division by zero.

Third Effort

In an attempt to answer the serious concern(s) raised during our first two efforts, we finally buckled down and performed the integrals necessary to determine expressions for key structural form factors in the cases where the internal structure is known analytically, specifically, for indexes <math>~n=5</math> and <math>~n=1</math>. The result is that the individual expressions derived by direct integration for <math>~\mathfrak{f}_W</math> and for <math>~\mathfrak{f}_A</math> do not match the general form-factor expressions that were rather cavalierly "derived" during our first effort. Oddly enough, as we discovered while fiddling around with the new results, the ratio of these form factors appears to be the same as before, namely,

<math>~\frac{\tilde\mathfrak{f}_W}{\tilde\mathfrak{f}_A - \tilde\theta^{n+1}}</math>

<math>~=</math>

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

It is worth noting that, as a result of this more thorough "third effort" examination, we have confirmed that the third key form factor,

<math>~\mathfrak{f}_M = \frac{\bar\rho}{\rho_c} = \biggl[- \frac{3\tilde\theta^'}{\tilde\xi}\biggr] \, ,</math>

which is the same as before and the same as for isolated polytropes. We also have determined that,

<math>~\biggl(\frac{M_\mathrm{limit}}{M_\mathrm{tot}}\biggr) \frac{1}{\mathfrak{f}_M} = \biggl(\frac{\tilde\xi^2 \tilde\theta^'}{\xi_1 \theta^'_1} \biggr)\biggl[- \frac{\tilde\xi}{3\tilde\theta^'}\biggr] = - \frac{\tilde\xi^3 }{3\xi_1 \theta^'_1} \, , </math>

except in the case of <math>~n=5</math> structures, for which we have determined,

<math>~\biggl[\biggl(\frac{M_\mathrm{limit}}{M_\mathrm{tot}}\biggr) \frac{1}{\mathfrak{f}_M} \biggr]_{n=5} = \ell^3 = \biggl( \frac{\tilde\xi^2}{3} \biggr)^{3/2} \, . </math>

First Effort, Second Time Around

In an accompanying chapter, we reproduce the discussion associated with our "First Effort", as referenced above, but correct expressions for <math>~\mathfrak{f}_W</math> and <math>~\mathfrak{f}_A</math>, as identified in our "Third Effort" and, accordingly, re-derive various affected expressions that follow.

Second Effort, Second Time Around

In an accompanying chapter, we reproduce the discussion associated with our "Second Effort", as referenced above, but revise key sections to incorporate corrected expressions for the structural form factors.

© 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