Revision as of 18:14, 24 April 2010

Massless Polytropic Tori

(aka Palapoizou-Pringle Tori)

In a seminal paper that focused on an analysis of nonaxisymmetric instabilities in accretion disks, Papaloizou & Pringle (1984, MNRAS, 208, 721-750; hereafter, PP84) began by constructing equilibrium structures of axisymmetric, polytropic tori that reside in (orbit about) a point-mass potential. The derived structures have analytic prescriptions. Although the tori constructed by PP84 were not self-gravitating — i.e., the tori were massless — it is nevertheless instructive for us to examine how these equilibrium structures were derived.

Governing Relations

As has been derived elsewhere, for axisymmetric configurations that obey a barotropic equation of state, hydrostatic balance is governed by the following algebraic expression:

<math>H + \Phi_\mathrm{eff} = C_\mathrm{B} ,</math>

where <math>C_\mathrm{B}</math> is the Bernoulli constant,

<math>\Phi_\mathrm{eff} \equiv \Phi + \Psi ,</math>

and <math>\Psi</math> is the relevant centrifugal potential. For self-gravitating configurations, this algebraic expression must be satisfied in concert with a self-consistent solution of the Poisson equation, but for the massless PP84 toroidal structures, <math>~\Phi</math> is just the Newtonian potential presented by a point-like object of mass <math>M_\mathrm{pt}</math>, namely,

<math>\Phi = - \frac{GM_\mathrm{pt}}{(\varpi^2 + z^2)^{1/2}} .</math>

Supplemental Relations

Following PP84, we supplement the above-specified set of governing equations with a polytropic equation of state, as defined in our overview of supplemental relations for time-independent problems. Specifically, we will assume that <math>~\rho</math> is related to <math>~H</math> through the relation,

<math>~H = (n+1)K_\mathrm{n} \rho^{1/n}</math> ,

or we can set,

Also following PP84, we impose a steady-state velocity flow-field that is described by a fluid with uniform specific angular momentum, <math>j_0</math>. Drawing from our table of example Simple rotation profiles, the centrifugal potential that describes this chosen flow-field is given by the expression,

<math> \Psi(\varpi) = \frac{j_0^2}{2\varpi^2} . </math>

Summary

In summary, for this problem the relevant simplified governing relation is,

<math> H = -\Phi_\mathrm{eff} + C_\mathrm{B} = \frac{GM_\mathrm{pt}}{(\varpi^2 + z^2)^{1/2}} - \Psi + C_\mathrm{B} . </math>

Inserting the two supplemental relations into this governing algebraic expression, we conclude that the polytropic tori studied by PP84 must have structures that satisfy the equation,

<math> (n+1)\frac{P}{\rho} = \frac{GM_\mathrm{pt}}{(\varpi^2 + z^2)^{1/2}} - \frac{j_0^2}{2\varpi^2} + C_\mathrm{B} . </math>

This is identical to Eq. (2.8) of PP84.

Solution

As PP84 point out, for these toroidal structures, it is convenient to normalize all lengths to the position in the equatorial plane, <math>\varpi_0</math>, at which a fluid particle with specific angular momentum <math>j_0</math> has an angular orbital frequency, <math>\dot\varphi = j_0/\varpi^2</math>, that matches the Keplerian orbital frequency,

<math> \omega_K \equiv \biggl[ \frac{GM_\mathrm{pt}}{\varpi^3} \biggr]^{1/2} , </math>

that is associated with the point-mass, <math>M_\mathrm{pt}</math>. That is, it is convenient to define the dimensionless coordinates,

<math> \chi \equiv \frac{\varpi}{\varpi_0} ~~~~~\mathrm{and}~~~~~ \zeta \equiv \frac{z}{\varpi_0} , </math>

where,

<math> \varpi_0 \equiv \frac{j_0^2}{GM_\mathrm{pt}} . </math>

The algebraic relation defining the equilibrium structure then becomes,

<math> H = (n+1)\frac{P}{\rho} = \frac{GM_\mathrm{pt}}{\varpi_0} \biggl[ (\chi^2 + \zeta^2)^{-1/2} - \frac{1}{2}\chi^{-2} - \frac{C_\mathrm{B} \varpi_0}{GM} \biggr] . </math>

Boundary Conditions

Given that it is a <math>2^\mathrm{nd}</math>-order ODE, a solution of the Lane-Emden equation will require specification of two boundary conditions. Based on our definition of the variable <math>\Theta_H</math>, one obvious boundary condition is to demand that <math>\Theta_H = 1</math> at the center (<math>\xi=0</math>) of the configuration. In astrophysically interesting structures, we also expect the first derivative of many physical variables to go smoothly to zero at the center of the configuration — see, for example, the radial behavior that was derived for <math>~P</math>, <math>~H</math>, and <math>~\Phi</math> in a uniform-density sphere. Hence, we will seek solutions to the Lane-Emden equation where <math>d\Theta_H /d\xi = 0</math> at <math>\xi=0</math> as well.

Related Wikipedia Discussions

Polytrope

@@ Line 61: / Line 61: @@
 </div>
 This is identical to Eq. (2.8) of PP84.
+==Solution==
 As PP84 point out, for these toroidal structures, it is convenient to normalize all lengths to the position in the equatorial plane, <math>\varpi_0</math>, at which a fluid particle with specific angular momentum <math>j_0</math> has an angular orbital frequency, <math>\dot\varphi = j_0/\varpi^2</math>, that matches the Keplerian orbital frequency,
@@ Line 80: / Line 84: @@
 </math>
 </div>
+The algebraic relation defining the equilibrium structure then becomes,
+<div align="center">
+<math>
+H = (n+1)\frac{P}{\rho} = \frac{GM_\mathrm{pt}}{\varpi_0} \biggl[ (\chi^2 + \zeta^2)^{-1/2} - \frac{1}{2}\chi^{-2}  - \frac{C_\mathrm{B} \varpi_0}{GM} \biggr] .
+</math>
+</div>
-==Solution==

Difference between revisions of "User:Tohline/Apps/PapaloizouPringleTori"