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

${\displaystyle P=K\rho ^{(n+1)/n},}$

Not to be confused with polytope.

The normalized density as a function of scale length for a wide range of polytropic indices

See also: Polytropic process

where P is pressure, ρ is density and K is a constant of proportionality.[1] The constant n is known as the polytropic index; note however that the polytropic index has an alternative definition as with n as the exponent.

This relation need not be interpreted as an equation of state, which states P as a function of both ρ and T (the temperature); however in the particular case described by the polytrope equation there are other additional relations between these three quantities, which together determine the equation. Thus, this is simply a relation that expresses an assumption about the change of pressure with radius in terms of the change of density with radius, yielding a solution to the Lane–Emden equation.

Sometimes the word polytrope may 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.

The polytropic exponent (of a polytrope) has been shown to be equivalent to the pressure derivative of the bulk modulus [2] where its relation to the Murnaghan equation of state has also been demonstrated. The polytrope relation is therefore best suited for relatively low-pressure (below 10⁷ Pa) and high-pressure (over 10¹⁴ Pa) conditions when the pressure derivative of the bulk modulus, which is equivalent to the polytrope index, is near constant.

Example models by polytropic index

Density (normalized to average density) versus radius (normalized to external radius) for a polytrope with index n=3.

• An index n = 0 polytrope is often used to model rocky planets as well.
• Neutron stars are well modeled by polytropes with index between n = 0.5 and n = 1.
• A polytrope with index n = 1.5 is a good model for fully convective star cores[3][4](like those of red giants), brown dwarfs, giant gaseous planets (like Jupiter). With this index, the polytropic exponent is 5/3, which is the heat capacity ratio (γ) for monoatomic gas. For the interior of gaseous stars (consisting of either ionized hydrogen or helium), this follows from an ideal gas approximation for natural convection conditions.
• A polytrope with index n = 1.5 is also a good model for white dwarfs of low mass, according to the equation of state of non-relativistic degenerate matter.[5]
• A polytrope with index n = 3 is a good model for the cores of white dwarfs of higher masses, according to the equation of state of relativistic degenerate matter.[5]
• A polytrope with index n = 3 is usually also used to model main-sequence stars like our Sun, at least in the radiation zone, corresponding to the Eddington standard model of stellar structure.[6]
• 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 Arthur Schuster in 1883, and it has an exact solution.
• A polytrope with index n = ∞ corresponds to what is called an isothermal sphere, that is an isothermal self-gravitating sphere of gas, whose structure is identical to the structure of a collisionless system of stars like a globular cluster. This is because for an ideal gas, the temperature is proportional to ρ^1/n, so infinite n corresponds to a constant temperature.

In general as the polytropic index increases, the density distribution is more heavily weighted toward the center (r = 0) of the body.

References

1. Horedt, G. P. (2004). Polytropes. Applications in Astrophysics and Related Fields, Dordrecht: Kluwer. ISBN 1-4020-2350-2
2. Weppner, S. P., McKelvey, J. P., Thielen, K. D. and Zielinski, A. K., "A variable polytrope index applied to planet and material models", Monthly Notices of the Royal Astronomical Society, Vol. 452, No. 2 (Sept. 2015), pages 1375–1393, Oxford University Press also found at the arXiv
3. S. Chandrasekhar [1939] (1958). An Introduction to the Study of Stellar Structure, New York: Dover. ISBN 0-486-60413-6
4. C. J. Hansen, S. D. Kawaler, V. Trimble (2004). Stellar Interiors – Physical Principles, Structure, and Evolution, New York: Springer. ISBN 0-387-20089-4
5. Sagert, I., Hempel, M., Greiner, C., Schaffner-Bielich, J. (2006). Compact stars for undergraduates. European journal of physics, 27(3), 577.
6. O. R. Pols (2011), Stellar Structure and Evolution, Astronomical Institute Utrecht, September 2011, pp. 64-68

See also

• Polytropic process
• Equation of state
• Murnaghan equation of state