Math 2.0

Integral equations Wiener-Hopf equations Example

Chandrasekhar's H-function

Builds on Radiative transfer equationMilne problemNonlinear integral equation

Example

Let Ψ\Psi be an even polynomial in μ\mu, the characteristic function, with Ψ≥0\Psi \ge 0 on [0,1][0, 1] and ∫01Ψ(μ) dμ≤12\int_0^1 \Psi(\mu)\, d\mu \le \frac{1}{2}. Chandrasekhar's H-function is the solution HH on [0,1][0, 1] of H(μ)=1+μ H(μ)∫01Ψ(μ′) H(μ′)μ+μ′ dμ′.H(\mu) = 1 + \mu\, H(\mu) \int_0^1 \frac{\Psi(\mu')\, H(\mu')}{\mu + \mu'}\, d\mu'. One takes the solution that is analytic in μ\mu in the right half-plane and continuous on [0,1][0, 1]. The simplest case is isotropic scattering, Ψ=ω02\Psi = \frac{\omega_0}{2} with albedo 0<ω0≤10 < \omega_0 \le 1. The unknown appears in a product with itself, so this is a nonlinear integral equation.

Check of a moment identity. Let I=∫01Ψ(μ)H(μ) dμI = \int_0^1 \Psi(\mu) H(\mu)\, d\mu. Multiply the equation by Ψ(μ)\Psi(\mu) and integrate over [0,1][0, 1]. The double integral ∫01∫01μμ+μ′ Ψ(μ)H(μ) Ψ(μ′)H(μ′) dμ′ dμ\int_0^1 \int_0^1 \frac{\mu}{\mu + \mu'}\, \Psi(\mu) H(\mu)\, \Psi(\mu') H(\mu')\, d\mu'\, d\mu does not change when μ\mu and μ′\mu' swap, so it equals half the integral with μ+μ′μ+μ′=1\frac{\mu + \mu'}{\mu + \mu'} = 1, that is 12I2\frac{1}{2} I^2. So I=∫01Ψ dμ+12I2I = \int_0^1 \Psi\, d\mu + \frac{1}{2} I^2, and the physical root is ∫01Ψ(μ)H(μ) dμ=1−1−2∫01Ψ(μ) dμ.\int_0^1 \Psi(\mu) H(\mu)\, d\mu = 1 - \sqrt{1 - 2 \int_0^1 \Psi(\mu)\, d\mu}. In the conservative case Ψ=12\Psi = \frac{1}{2} this gives ∫01H(μ) dμ=2\int_0^1 H(\mu)\, d\mu = 2. Also H(0)=1H(0) = 1, directly from the equation.

Remarks

The function HH is tied to a Wiener–Hopf factorization. For zz off the segment [−1,1][-1, 1], with the analytic continuation of HH, one has 1H(z) H(−z)=1−2z2∫01Ψ(μ)z2−μ2 dμ.\frac{1}{H(z)\, H(-z)} = 1 - 2 z^2 \int_0^1 \frac{\Psi(\mu)}{z^2 - \mu^2}\, d\mu. The right side is the dispersion function of the radiative transfer equation in a half-space; H(−z)H(-z) is the factor holomorphic for Re⁡z<0\operatorname{Re} z < 0 and H(z)H(z) the factor holomorphic for Re⁡z>0\operatorname{Re} z > 0. As z→∞z \to \infty, both sides tend to 1−2∫01Ψ dμ1 - 2\int_0^1 \Psi\, d\mu, consistent with H(∞)=1/(1−I)H(\infty) = 1/(1 - I) from the equation. In the conservative case, HH gives the exact angular distribution of the light leaving a grey atmosphere, the companion of the Milne problem.

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  1. Exponential integral concept
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  5. Wiener–Hopf method concept
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  7. Chandrasekhar's H-function example

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Further reading

  1. Web https://en.wikipedia.org/wiki/Chandrasekhar%27s_H-function
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Tag99879Z5Y1K
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Kindexample
WritingW0 stub
MSC45G10, 85A25, 45E10
Instance ofNonlinear integral equation
UsesRadiative transfer equation, Milne problem, Nonlinear integral equation
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