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Context

Global Energy Considerations

Principal Governing Equations (PGEs)		Continuity		Euler		1st Law of Thermodynamics		Poisson

 

Equation of State (EOS)		Ideal Gas		Total Pressure   Bond, Arnett, & Carr (1984)

Spherically Symmetric Configurations

(Initially) Spherically Symmetric Configurations

 

		Structural Form Factors		Free-Energy of Spherical Systems

One-Dimensional PGEs

Equilibrium Structures

1D STRUCTURE

 

		Scalar Virial Theorem

Hydrostatic Balance Equation		$\frac{dP}{dr}=-\frac{G{M}_r\rho }{r^2}$		Solution Strategies

Uniform-Density Sphere

 

Isothermal Sphere		$\frac{1}{{\xi }^2}\frac{d}{d\xi }\left({\xi }^2\frac{d\psi }{d\xi }\right)=e^{-\psi }$		via Direct Numerical Integration

Isolated Polytropes		Lane (1870)		$\frac{1}{{\xi }^2}\frac{d}{d\xi }\left({\xi }^2\frac{d{\mathrm{\Theta }}_H}{d\xi }\right)=-{\mathrm{\Theta }}_H^n$		Known Analytic Solutions		via Direct Numerical Integration		via Self-Consistent Field (SCF) Technique

 

Zero-Temperature White Dwarf		Chandrasekhar Limiting Mass (1935)

Virial Equilibrium of Pressure-Truncated Polytropes

Pressure-Truncated Configurations		Bonnor-Ebert (Isothermal) Spheres (1955 - 56)		Embedded Polytropes		Equilibrium Sequence Turning-Points ♥				Turning-Points (Broader Context)

Free Energy of Bipolytropes (nc, ne) = (5, 1)

Composite Polytropes (Bipolytropes)		Milne (1930)		Schönberg- Chandrasekhar Mass (1942)		Murphy (1983) Analytic (nc, ne) = (1, 5)		Eggleton, Faulkner & Cannon (1998) Analytic (nc, ne) = (5, 1)

Stability Analysis

1D STABILITY

Three different approaches are used in the study of hydrodynamical stability of stars and other gravitating objects …  

• The first approach is based on the use of the equations of small oscillations. In that case the problem is reduced to a search for the solution of the boundary-value problem of the Stourme-Liuville type for the linearised system of equations of small oscillations. The solutions consist of a set of eigenfrequencies and eigenfunctions. The following set of menu tiles include links to chapters where this approach has been applied to: (a) uniform-density configurations, (b) pressure-truncated isothermal spheres, (c) an isolated n = 3 polytrope, (d) pressure-truncated n = 5 configurations, and (e) bipolytropes having $(n_c,n_e)=(1,5)$.
• Second, one can derive a variational principle from the equations of small oscillations. Below, an appropriately labeled (purple) menu tile links to a chapter in which the foundation for this approach is developed. With the aid of the variational principle, the problem is reduced to the search of the best trial functions; this leads to approximate eigenvalues of oscillations. In spite of the simplifications introduced by the use of the variational principle and by not solving the equations of motion exactly, the problem still remains complicated … One menu tile, below, links to a chapter in which an analytic (exact) demonstration of the variational principle's utility is provided in the context pressure-truncated n = 5 polytropes.
• The third approach is what we have already referred to as a free-energy — and associated virial theorem — analysis. When this method is used, it is not necessary to use the equations of small oscillations but, instead, the functional expression for the total energy of the momentarily stationary (but not necessarily in equilibrium) star is sufficient. The condition that the first variation of the energy vanishes, determines the state of equilibrium of the star and the positiveness of a second variation indicates stability.

If one wants to know from a stability analysis the answer to only one question — whether the model is stable or not — then the most straightforward procedure is to use the third, static method … For the application of this method, one needs to construct only equilibrium, stationary models, with no further calculation. Generally the static analysis gives no information about the shape of the modes of oscillation, but, in the vicinity of critical points, where instability sets in, this method makes it possible to find the eigenfunction of the mode which becomes unstable at the critical point. Generally in what follows, this will be referred to as the "B-KB74 conjecture;" a menu tile carrying this label is linked to a chapter in which this approach is used to analyze the onset of a dynamical instability along the equilibrium sequence of pressure-truncated n = 5 polytropes.

--- Text in green taken directly from G. S. Bisnovatyi-Kogan & S. I. Blinnikov (1974); B-KB74, for short.

 
 

		Variational Principle

Radial Pulsation Equation		Example Derivations & Statement of Eigenvalue Problem		(poor attempt at) Reconciliation		Relationship to Sound Waves

 

Jeans (1928) or Bonnor (1957)		Ledoux & Walraven (1958)		Rosseland (1969)

 

Uniform-Density Configurations		Sterne's Analytic Sol'n of Eigenvalue Problem (1937)

 

Pressure-Truncated Isothermal Spheres		$0=\frac{d^{2}x}{d{\xi }^2}+[4-\xi (\frac{d\psi }{d\xi }\left)\right]\frac{1}{\xi }\cdot \frac{dx}{d\xi }+\left[\right(\frac{{\sigma }_c^2}{6{\gamma }_{\mathrm{g}}}){\xi }^2-\alpha \xi (\frac{d\psi }{d\xi }\left)\right]\frac{x}{{\xi }^2}$ where:    ${\sigma }_c^2\equiv \frac{3{\omega }^2}{2\pi G{\rho }_c}$     and,     $\alpha \equiv (3-\frac{4}{{\gamma }_{\mathrm{g}}})$		via Direct Numerical Integration

 

Yabushita's Analytic Sol'n for Marginally Unstable Configurations (1974)		${\sigma }_c^2=0,{\gamma }_{\mathrm{g}}=1$  and   $x=1-\left(\frac{1}{\xi e^{-\psi }}\right)\frac{d\psi }{d\xi }$

 

Polytropes		$0=\frac{d^{2}x}{d{\xi }^2}+[4-(n+1)Q]\frac{1}{\xi }\cdot \frac{dx}{d\xi }+(n+1)\left[\right(\frac{{\sigma }_c^2}{6{\gamma }_g})\frac{{\xi }^2}{\theta }-\alpha Q]\frac{x}{{\xi }^2}$ where:    $Q(\xi )\equiv -\frac{d\ln \theta }{d\ln \xi },$    ${\sigma }_c^2\equiv \frac{3{\omega }^2}{2\pi G{\rho }_c},$     and,     $\alpha \equiv (3-\frac{4}{{\gamma }_{\mathrm{g}}})$		Isolated n = 3 Polytrope

Exact Demonstration of B-KB74 Conjecture		Exact Demonstration of Variational Principle

Pressure-Truncated n = 5 Configurations

Our (2017) Analytic Sol'n for Marginally Unstable Configurations ♥		${\sigma }_c^2=0,{\gamma }_{\mathrm{g}}=(n+1)/n$  and   $x=\frac{3(n-1)}{2n}[1+(\frac{n-3}{n-1}\left)\right(\frac{1}{\xi {\theta }^n}\left)\frac{d\theta }{d\xi }\right]$

 

B-KB74 Conjecture RE: Bipolytrope (nc, ne) = (5, 1)

BiPolytropes		Murphy & Fiedler (1985b) (nc, ne) = (1,5)		Our Broader Analysis

Nonlinear Dynamical Evolution

1D DYNAMICS

 

Free-Fall Collapse

 

Collapse of Isothermal Spheres		via Direct Numerical Integration		Similarity Solution

 

Collapse of an Isolated n = 3 Polytrope

 

Two-Dimensional Configurations (Axisymmetric)

(Initially) Axisymmetric Configurations

 

Storyline

 

PGEs for Axisymmetric Systems

Axisymmetric Equilibrium Structures

2D STRUCTURE

 

Constructing Steady-State Axisymmetric Configurations		Axisymmetric Instabilities to Avoid		Simple Rotation Profiles		Hachisu Self-Consistent-Field [HSCF] Technique		Solving the Poisson Equation

 

Using Toroidal Coordinates to Determine the Gravitational Potential				Attempt at Simplification ♥		Wong's Analytic Potential (1973)

Spheroidal & Spheroidal-Like

Uniform-Density (Maclaurin) Spheroids		Maclaurin's Original Text & Analysis (1742)				Maclaurin Spheroid Sequence

 

Rotationally Flattened Isothermal Configurations		Hayashi, Narita & Miyama's Analytic Sol'n (1982)		Review of Stahler's (1983) Sol'n Technique

 

Rotationally Flattened Polytropes		Example Equilibria

 

Rotationally Flattened White Dwarfs		Ostriker Bodenheimer & Lynden-Bell (1966)		Example Equilibria

Toroidal & Toroidal-Like

 

Massless Polytropic Configurations		Papaloizou-Pringle Tori (1984)

 

Self-Gravitating Incompressible Configurations		Dyson (1893)		Dyson-Wong Tori

 

Self-Gravitating Compressible Configurations		Ostriker (1964)

 

See Also