Difference between revisions of "User:Tohline/Apps/ReviewStahler83"

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==Governing Equations==
==Governing Equations==


[http://adsabs.harvard.edu/abs/1983ApJ...268..155S Stahler (1983a)] states that the <font color="darkgreen">equilibrium configuration is found by solving the equation for momentum balance together with Poisson's equation for the gravitational potential</font>, <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),
[http://adsabs.harvard.edu/abs/1983ApJ...268..155S Stahler (1983a)] states that the <font color="darkgreen">equilibrium configuration is found by solving the equation for momentum balance together with Poisson's equation for the gravitational potential</font>, <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, but note the sign change and "pink comment" shown here on the right),
<div align="center" id="GravitationalPotential">
<div align="center" id="GravitationalPotential">
[[File:CommentButton02.png|right|100px|Note from J. E. Tohline:  As is written here and in eq. (A1) of Stahler's (1983a) ''Appendix A'', a negative sign explicitly appears on the right-hand-side of the integral form of Poisson's equation.  In contrast to this, the right-hand side of Stahler's eq. (10) is explicitly positive.  We suspect that the absence of negative sign in Stahler's eq. (10) is a typographical error.]]
[[File:CommentButton02.png|right|100px|Note from J. E. Tohline:  As is written here and in eq. (A1) of Stahler's (1983a) ''Appendix A'', a negative sign explicitly appears on the right-hand-side of the integral form of Poisson's equation.  In contrast to this, the right-hand side of Stahler's eq. (10) is explicitly positive.  We suspect that the absence of negative sign in Stahler's eq. (10) is a typographical error.]]
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Except for the overall sign, this matches the expression for the '''[[User:Tohline/SR/PoissonOrigin#Step_1|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>.
As is clear from our [[User:Tohline/SR/PoissonOrigin#Step_1|separate discussion of the origin of Poisson's equation]], this matches the expression for the scalar gravitational potential that is widely used in astrophysics.   


Working in cylindrical coordinates <math>~(\varpi, z)</math> &#8212; as we have [[User:Tohline/AxisymmetricConfigurations/PGE#Axisymmetric_Configurations_.28Part_I.29|explained elsewhere]], the assumption of axisymmetry eliminates the azimuthal angle &#8212; Stahler states that <font color="darkgreen">the momentum equation is</font> (see his equation 2):
Working in cylindrical coordinates <math>~(\varpi, z)</math> &#8212; as we have [[User:Tohline/AxisymmetricConfigurations/PGE#Axisymmetric_Configurations_.28Part_I.29|explained elsewhere]], the assumption of axisymmetry eliminates the azimuthal angle &#8212; Stahler states that <font color="darkgreen">the momentum equation is</font> (see his equation 2):
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where, <math>~\nabla \equiv (\partial/\partial\varpi, \partial/\partial z)</math>, and the centrifugal potential is given by (see Stahler's equation 3):
where, <math>~\nabla \equiv (\partial/\partial\varpi, \partial/\partial z)</math>, and the centrifugal potential is given by (see Stahler's equation 3, but note the sign change and "pink comment" shown here on the right):
<div align="center">
<div align="center">
[[File:CommentButton02.png|right|100px|Note from J. E. Tohline:  As is written here and in the definition of &Psi; that accompanies our separate discussion of ''simple rotation profiles'', a negative sign explicitly appears in the integral expression for the centrifugal potential.  In contrast to this, the right-hand side of Stahler's eq. (3) is explicitly positive.  We suspect that the absence of a negative sign in Stahler's eq. (3) is a typographical error.]]
[[File:CommentButton02.png|right|100px|Note from J. E. Tohline:  As is written here and in the definition of &Psi; that accompanies our separate discussion of ''simple rotation profiles'', a negative sign explicitly appears in the integral expression for the centrifugal potential.  In contrast to this, the right-hand side of Stahler's eq. (3) is explicitly positive.  We suspect that the absence of a negative sign in Stahler's eq. (3) is a typographical error.]]
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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 [[User:Tohline/AxisymmetricConfigurations/SolutionStrategies#Simple_Rotation_Profile_and_Centrifugal_Potential|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 <font color="darkgreen">that <math>~j</math> is not a function of <math>~z</math></font>; this builds in the physical constraint enunciated by the [[User:Tohline/2DStructure/AxisymmetricInstabilities#Poincar.C3.A9-Wavre_Theorem|Poincar&eacute;-Wavre theorem]], <font color="darkgreen">which guarantees that rotational velocity is constant on cylinders for the equilibrium of any barotropic fluid</font>.
where <math>~j</math> is the z-component of the angular momentum per unit mass.  This last expression is precisely the same expression for the centrifugal potential that we [[User:Tohline/AxisymmetricConfigurations/SolutionStrategies#Simple_Rotation_Profile_and_Centrifugal_Potential|have defined in the context of our discussion of ''simple rotation profiles]].'' As Stahler stresses, by adopting a centrifugal potential of this form, he is implicitly assuming <font color="darkgreen">that <math>~j</math> is not a function of <math>~z</math></font>; this builds in the physical constraint enunciated by the [[User:Tohline/2DStructure/AxisymmetricInstabilities#Poincar.C3.A9-Wavre_Theorem|Poincar&eacute;-Wavre theorem]], <font color="darkgreen">which guarantees that rotational velocity is constant on cylinders for the equilibrium of any barotropic fluid</font>.


As we have demonstrated in our [[User:Tohline/AxisymmetricConfigurations/SolutionStrategies#2DgoverningEquations|overview discussion of axisymmetric configurations]], the equations that govern the equilibrium properties of axisymmetric structures are,
As we have demonstrated in our [[User:Tohline/AxisymmetricConfigurations/SolutionStrategies#2DgoverningEquations|overview discussion of axisymmetric configurations]], the equations that govern the equilibrium properties of axisymmetric structures are,

Revision as of 03:19, 4 April 2018

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).


Whitworth's (1981) Isothermal Free-Energy Surface
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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, but note the sign change and "pink comment" shown here on the right),

Note from J. E. Tohline: As is written here and in eq. (A1) of Stahler's (1983a) Appendix A, a negative sign explicitly appears on the right-hand-side of the integral form of Poisson's equation. In contrast to this, the right-hand side of Stahler's eq. (10) is explicitly positive. We suspect that the absence of negative sign in Stahler's eq. (10) is a typographical error.

<math>~ \Phi_g(\vec{x})</math>

<math>~=</math>

<math>~ - G \int \frac{\rho(\vec{x}^{~'})}{|\vec{x}^{~'} - \vec{x}|} d^3x^' \, .</math>

As is clear from our separate discussion of the origin of Poisson's equation, this matches the expression for the scalar gravitational potential that is widely used in astrophysics.

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):

<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, but note the sign change and "pink comment" shown here on the right):

Note from J. E. Tohline: As is written here and in the definition of Ψ that accompanies our separate discussion of simple rotation profiles, a negative sign explicitly appears in the integral expression for the centrifugal potential. In contrast to this, the right-hand side of Stahler's eq. (3) is explicitly positive. We suspect that the absence of a negative sign in Stahler's eq. (3) is a typographical error.

<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. 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. 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,

<math>~ \biggl[ \frac{1}{\rho}\frac{\partial P}{\partial\varpi} + \frac{\partial \Phi}{\partial\varpi}\biggr] - \frac{j^2}{\varpi^3} </math>

<math>~=</math>

<math>~0 \, ,</math>

<math>~ \biggl[ \frac{1}{\rho}\frac{\partial P}{\partial z} + \frac{\partial \Phi}{\partial z} \biggr] </math>

<math>~=</math>

<math>~0 \, ,</math>

<math>~ \frac{1}{\varpi} \frac{\partial }{\partial\varpi} \biggl[ \varpi \frac{\partial \Phi}{\partial\varpi} \biggr] + \frac{\partial^2 \Phi}{\partial z^2} </math>

<math>~=</math>

<math>~4\pi G \rho \, .</math>

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 explored, we have followed Shu's (1992) lead and have derived what we have referred to as a,

Generalized Scalar Virial Theorem

<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>

Shu92, p. 331, Eq. (24.12)

Recognizing that,

<math>~2S_\mathrm{therm} = 3 \int_V P d^3x \, ,</math>

and ignoring magnetic field effects — that is, zeroing out <math>~\mathcal{M}</math> and the surface integral involving <math>~\overrightarrow{T}</math> — this generalized scalar virial theorem becomes,

<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,


Whitworth's (1981) Isothermal Free-Energy Surface

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