POLYTROPE

In astrophysics, a 'polytrope' refers to a solution of the Lane-Emden equation in which the pressure depends upon the density in the form $P\; =\; K$
ho^{((n+1)/n)}, where $P$ is pressure, $$
ho is density and $K$ is a constant. The constant $n$ is known as the polytropic index. This relation need not be interpreted as an equation of state, although a gas following such an equation of state does indeed produce a polytropic solution to the Lane-Emden equation. Rather, this is simply a relationship that expresses an assumption regarding the evolution of $P$ with radius, in terms of the evolution of $$
ho with radius, yielding a solution to the Lane-Emden equation.
For example, given an ideal gas and given a polytropic index, the constant $K$ is
$$
K = left({ rac{N_A k_B T}{mu}}
ight)
ho^{-1/n}

and the expression on the right hand side is, for whatever reason, assumed to be constant throughout the solution.

A polytrope with index n=0 has a uniform density.
Neutron stars are well modeled by polytropes with index about in the range between n=0.5 and n=1.
A polytrope with index n=3/2 is a good model for degenerate star cores ( like those of red giants ), for white dwarfs, brown dwarfs, giant gaseous planets ( like Jupiter ), or even for rocky planets.

Main sequence stars like our Sun are usually modeled by a polytrope with index n=3, corresponding to the Eddington standard model of stellar structure.
A polytrope with index n=5 has an infinite radius. It corresponds to the simplest plausible model of a self-consistent stellar system, first studied by A. Schuster in 1883.

A polytrope with index $n=infty$ corresponds to what is called ''isothermal sphere'', that is an isothermal self-gravitating sphere of gas, whose structure is identical with the structure of a collisionless system of stars like a globular cluster.
Note that the higher the polytropic index, the more condensed at the centre is the density distribution.
Sometimes the word ''polytrope'' may be used to refer to an equation of state that looks similar to the thermodynamic relation above, although this is potentially confusing and is to be avoided. It is preferable to refer to the fluid itself (as opposed to the solution of the Lane-Emden equation) as a polytropic fluid. The equation of state of a polytropic fluid is general enough that such idealized fluids find wide use outside of the limited problem of polytropes.

Contents

References

References

★ Chandrasekhar, S. [ 1939 ] ( 1958 ). ''An Introduction to the Study of Stellar Structure'', New York : Dover. ISBN 0-486-60413-6

★ Hansen, C.J., Kawaler S.D. & Trimble V. ( 2004 ). ''Stellar Interiors - Physical Principles, Structure, and Evolution'', New York : Springer. ISBN 0-387-20089-4

★ Horedt, G.P. ( 2004 ). ''Polytropes. Applications in Astrophysics and Related Fields'', Dordrecht : Kluwer. ISBN 1-4020-2350-2