Lane–Emden equation

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Solutions of Lane–Emden equation for n = 0, 1, 2, 3, 4, 5.

In astrophysics, the Lane–Emden equation is a dimensionless form of Poisson's equation for the gravitational potential of a Newtonian self-gravitating, spherically symmetric, polytropic fluid. It is named after astrophysicists Jonathan Homer Lane and Robert Emden.[1] The equation reads

 \frac{1}{\xi^2} \frac{d}{d\xi} \left({\xi^2 \frac{d\theta}{d\xi}}\right) + \theta^n = 0

where \xi is a dimensionless radius and \theta is related to the density (and thus the pressure) by \rho=\rho_c\theta^n for central density \rho_c. The index n is the polytropic index that appears in the polytropic equation of state,

 P = K \rho^{1 + \frac{1}{n}}\,

where P and \rho are the pressure and density, respectively, and K is a constant of proportionality. The standard boundary conditions are \theta(0)=1 and \theta'(0)=0. Solutions thus describe the run of pressure and density with radius and are known as polytropes of index n.


Physically, hydrostatic equilibrium connects the gradient of the potential, the density, and the gradient of the pressure, whereas Poisson's equation connects the potential with the density. Thus, if we have a further equation that dictates how the pressure and density vary with respect to one another, we can reach a solution. The particular choice of a polytropic gas as given above makes the mathematical statement of the problem particularly succinct and leads to the Lane–Emden equation. The equation is a useful approximation for self-gravitating spheres of plasma such as stars, but typically it is a rather limiting assumption.


From hydrostatic equilibrium[edit]

Consider a self-gravitating, spherically symmetric fluid in hydrostatic equilibrium. Mass is conserved and thus described by the continuity equation

 \frac{dm}{dr} = 4\pi r^2 \rho

where \rho is a function of r. The equation of hydrostatic equilibrium is

 \frac{1}{\rho}\frac{dP}{dr} = -\frac{Gm}{r^2}

where m is also a function of r. Differentiating again gives

\frac{d}{dr}\left(\frac{1}{\rho}\frac{dP}{dr}\right) &= \frac{2Gm}{r^3}-\frac{G}{r^2}\frac{dm}{dr} \\
&=-\frac{2}{\rho r}\frac{dP}{dr}-4\pi G\rho

where we have used the continuity equation to replace the mass gradient. Multiplying both sides by r^2 and collecting the derivatives of P on the left, we can write

=\frac{d}{dr}\left(\frac{r^2}{\rho}\frac{dP}{dr}\right)=-4\pi Gr^2\rho

Dividing both sides by r^2 yields, in some sense, a dimensional form of the desired equation. If, in addition, we substitute for the polytropic equation of state with P=K\rho_c^{1+\frac{1}{n}}\theta^{n+1} and \rho=\rho_c\theta^n, we have

 \frac{1}{r^2}\frac{d}{dr}\left(r^2K\rho_c^\frac{1}{n}(n+1)\frac{d\theta}{dr}\right)=-4\pi G\rho_c\theta^n

Gathering the constants and substituting r=\alpha\xi, where

\alpha^2=(n+1)K\rho_c^{\frac{1}{n}-1}/4\pi G,

we have the Lane–Emden equation,

 \frac{1}{\xi^2} \frac{d}{d\xi} \left({\xi^2 \frac{d\theta}{d\xi}}\right) + \theta^n = 0

From Poisson's equation[edit]

Equivalently, one can start with Poisson's equation,

 \nabla^2\Phi=\frac{1}{r^2}\frac{d}{dr}\left({r^2\frac{d\Phi}{dr}}\right) = 4\pi G\rho

We can replace the gradient of the potential using the hydrostatic equilibrium, via

 \frac{d\Phi}{dr}= - \frac{1}{\rho}\frac{dP}{dr}

which again yields the dimensional form of the Lane–Emden equation.


For a given value of the polytropic index n, denote the solution to the Lane–Emden equation as \theta_n(\xi). In general, the Lane–Emden equation must be solved numerically to find \theta_n. There are exact, analytic solutions for certain values of n, in particular: n = 0,1,5. For n between 0 and 5, the solutions are continuous and finite in extent, with the radius of the star given by R = \alpha \xi_1 , where \theta_n(\xi_1) = 0.

For a given solution \theta_n, the density profile is given by,

 \rho = \rho_c \theta_n^n

The total mass M of the model star can be found by integrating the density over radius, from 0 to \xi_1.

The pressure can be found using the polytropic equation of state, P = K \rho^{1+\frac{1}{n}} , i.e.

 P = K \rho_c^{1+\frac{1}{n}} \theta_n^{n+1}

Finally, if the gas is ideal, the equation of state is P = k_B\rho T/\mu, where k_B is the Boltzmann constant and m the mean molecular weight. The temperature profile is then given by

 T = \frac{K\mu}{k_B} \rho_c^{1/n} \theta_n

Exact Solutions[edit]

There are only three values of the polytropic index n that lead to exact solutions.

For n = 0[edit]

If n=0, the equation becomes

 \frac{1}{\xi^2} \frac{d}{d\xi} \left({\xi^2 \frac{d\theta}{d\xi}}\right) + 1 = 0

Re-arranging and integrating once gives

 \xi^2\frac{d\theta}{d\xi} = C_1-\frac{1}{3}\xi^3

Dividing both sides by \xi^2 and integrating again gives


The boundary conditions \theta(0)=1 and \theta'(0)=0 imply that the constants of integration are C_0=1 and C_1=0.

For n = 1[edit]

When n=1, the equation can be expanded in the form

 \frac{d^2\theta}{d\xi^2}+\frac{2}{\xi}\frac{d\theta}{d\xi} + \theta = 0

We assume a power series solution:

 \theta(\xi)=\sum\limits_{n=0}^\infty a_n \xi^n

This leads to a recursive relationship for the expansion coefficients:

 a_{n+2} = -\frac{a_n}{(n+3)(n+2)}

This relation can be solved leading to the general solution:

 \theta(\xi)=a_0 \frac{\sin\xi}{\xi} + a_1 \frac{\cos\xi}{\xi}

The boundary condition for a physical polytrope demands that  \theta(\xi) \rightarrow 1 as  \xi \rightarrow 0 . This requires that  a_0 = 1, a_1 = 0 , thus leading to the solution:


For n = 5[edit]

After a sequence of substitutions, it can be shown that the Lane–Emden equation has a further solution


when n=5. This solution is finite in mass but infinite in radial extent, and therefore the complete polytrope does not represent a physical solution.

Numerical Solutions[edit]

In general, solutions are found by numerical integration. Many standard methods require that the problem is formulated as a system of first-order ordinary differential equations. For example,


Here, \phi(\xi) is interpreted as the dimensionless mass, defined by m(r)=4\pi\alpha^3\rho_c\phi(\xi). The relevant initial conditions are \phi(0)=0 and \theta(0)=1. The first equation represents hydrostatic equilibrium and the second represents mass conservation.

Homologous Variables[edit]

Homology-invariant equation[edit]

It is known that if \theta(\xi) is a solution of the Lane–Emden equation, then so is C^{2/n+1}\theta(C\xi).[2] Solutions that are related in this way are called homologous; the process that transforms them is homology. If we choose variables that are invariant to homology, then we can reduce the order of the Lane–Emden equation by one.

A variety of such variables exist. A suitable choice is

U=\frac{d\log m}{d\log r}=\frac{\xi^3\theta^n}{\phi}


V=\frac{d\log P}{d\log r}=(n+1)\frac{\phi}{\xi\theta}

We can differentiate the logarithms of these variables with respect to \xi, which gives




Finally, we can divide these two equations to eliminate the dependence on \xi, which leaves


This is now a single first-order equation.

Topology of the homology-invariant equation[edit]

The homology-invariant equation can be regarded as the autonomous pair of equations




The behaviour of solutions to these equations can be determined by linear stability analysis. The critical points of the equation (where dV/d\log\xi=dU/d\log\xi=0) and the eigenvalues and eigenvectors of the Jacobian matrix are tabulated below.[3]

Critical point Eigenvalues Eigenvectors
(0,0) 3 -1 (1,0) (0,1)
(3,0) -3 2 (1,0) (-3n,5+5n)
(0,n+1) 1 3-n (0,1) (2-n,1+n)
\left(\frac{n-3}{n-1},2\frac{n+1}{n-1}\right) \frac{n-5\pm\Delta_n}{2-2n} \left(1-n\mp\Delta_n,4+4n\right)

Further reading[edit]

Horedt, Georg P. (2004). Polytropes - Applications in Astrophysics and Related Fields. Dordrecht: Kluwer Academic Publishers. ISBN 978-1-4020-2350-7. 


  1. ^ Lane, Jonathan Homer (1870). "On the Theoretical Temperature of the Sun under the Hypothesis of a Gaseous Mass Maintaining its Volume by its Internal Heat and Depending on the Laws of Gases Known to Terrestrial Experiment". The American Journal of Science and Arts. 2 50: 57–74. 
  2. ^ Chandrasekhar, Subrahmanyan (1939). An introduction to the study of stellar structure. Chicago, Ill.: University of Chicago Press. 
  3. ^ Horedt, Georg P. (1987). "Topology of the Lane-Emden equation". Astronomy and Astrophysics 117 (1-2): 117–130. Bibcode:1987A&A...177..117H. 

External links[edit]