User:Tohline/Apps/ReviewStahler83
Stahler's (1983) Rotationally Flattened Isothermal Configurations
Consider the collapse of an isothermal cloud (characterized by isothermal sound speed, <math>~c_s</math>) that is initially spherical, uniform in density, uniformly rotating <math>~(\Omega_0)</math>, and embedded in a tenuous intercloud medium of pressure, <math>~P_e</math>. Now suppose that the cloud maintains perfect axisymmetry as it collapses and that <math>~c_s</math> never changes at any fluid element. To what equilibrium state will this cloud collapse if the specific angular momentum of every fluid element is conserved? In a paper titled, The Equilibria of Rotating, Isothermal Clouds. I. - Method of Solution, S. W. Stahler (1983a, ApJ, 268, 155 - 184) describes a numerical scheme — a self-consistent-field technique — that he used to construct such equilibrium states.
In what follows, lines of text that appear in a dark green font have been extracted verbatim from Stahler (1983a).
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Governing Equations
Stahler (1983a) states that the equilibrium configuration is found by solving the equation for momentum balance together with Poisson's equation for the gravitational potential, <math>~\Phi_g</math>. Stahler chooses to use the integral form of Poisson's equation to define the gravitational potential, namely (see his equation 10),
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<math>~ \Phi_g(\vec{x})</math> |
<math>~=</math> |
<math>~ G \int \frac{\rho(\vec{x}^{~'})}{|\vec{x}^{~'} - \vec{x}|} d^3x^' \, .</math> |
Except for the overall sign, this matches the expression for the Scalar Gravitational Potential that is widely used in astrophysics. So a mapping from his notation to ours is accomplished via the substitution, <math>~\Phi_g \rightarrow -\Phi</math>.
Working in cylindrical coordinates <math>~(\varpi, z)</math> — as we have explained elsewhere, the assumption of axisymmetry eliminates the azimuthal angle — Stahler states that the momentum equation is (see his equation 2):
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<math>~\frac{\nabla P}{\rho} + \nabla\Phi_g + \nabla\Phi_c</math> |
<math>~=</math> |
<math>~0 \, ,</math> |
where, <math>~\nabla \equiv (\partial/\partial\varpi, \partial/\partial z)</math>, and the centrifugal potential is given by (see Stahler's equation 3):
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<math>~\Phi_c(\varpi)</math> |
<math>~\equiv</math> |
<math>~ \int_0^\varpi \frac{j^2(\varpi^') d\varpi^'}{(\varpi^')^3} \, , </math> |
where <math>~j</math> is the z-component of the angular momentum per unit mass. Except for the overall sign, this last expression is precisely the same expression for the centrifugal potential that we have defined in the context of our discussion of simple rotation profiles, so in this context a mapping from Stahler's notation to ours is accomplished via the substituion, <math>~\Phi_c \rightarrow - \Psi</math>. As Stahler stresses, by adopting a centrifugal potential of this form, he is implicitly assuming that <math>~j</math> is not a function of <math>~z</math>; this builds in the physical constraint enunciated by the Poincaré-Wavre theorem, which guarantees that rotational velocity is constant on cylinders for the equilibrium of any barotropic fluid.
As we have demonstrated in our overview discussion of axisymmetric configurations, the equations that govern the equilibrium properties of axisymmetric structures are,
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Let's compare this set of governing equations with the ones used by Stahler (1983a).
Scalar Virial Theorem
In an accompanying chapter where global energy considerations are discussed, we have followed Shu's (1992) lead and have derived what we have referred to as a,
Generalized Scalar Virial Theorem
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<math>~~2 (T_\mathrm{kin} + S_\mathrm{therm}) + W_\mathrm{grav} + \mathcal{M}</math> |
<math>~=</math> |
<math> ~P_e \oint \vec{x}\cdot \hat{n} dA - \oint \vec{x}\cdot \overrightarrow{T}\hat{n} dA \, .</math> |
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Shu92, p. 331, Eq. (24.12) |
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<math>~2S_\mathrm{therm} = 3 \int_V P d^3x \, ,</math>
and ignoring magnetic field effects — specifically, <math>~\mathcal{M}</math>, and the surface integral involving <math>~\overrightarrow{T}</math> — this generalized scalar virial theorem becomes,
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<math>~~2 T_\mathrm{kin} + 3 \int_V P d^3x + W_\mathrm{grav} </math> |
<math>~=</math> |
<math> ~P_e \oint \vec{x}\cdot \hat{n} dA \, .</math> |
This exactly matches Stahler's expression for the scalar virial theorem (see his equation 16), if the external pressure, <math>~P_e</math>, is assumed to be uniform across the surface of the equilibrium configuration.
Solution Technique
Following exactly along the lines of the HSCF technique that has been described in an accompanying chapter,
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