A problem in radiative transfer theory concerning the single-velocity kinetic transport equation of quanta or particles in a half-space. The integral equation of the Milne problem with a source at infinity under zero incident flux of the radiation was first introduced by E. Milne  for the case of isotropic scattering of quanta, diffusing without absorption in a stellar atmosphere.
The Milne equation takes the form
Here is the radiation (or particle) density and
is the exponential integral function .
In neutron physics the Milne problem is used for the formulation of approximate boundary conditions for solutions of the equations of a diffusion approximation in a bounded domain; in this connection one takes into account neutron capture by the medium, anisotropic scattering and the curvature of the boundary.
Here the Milne problem is to solve the integro-differential equation
with boundary conditions on the boundary of the half-space occupied by the matter, with a vacuum
where is the mean number of secondary neutrons, colliding once with a nucleus ( for scattering and absorbing neutrons by the medium), and is the indicatrix of the scattering ( for isotropic scattering). The spherical or cylindrical Milne problem on the distribution of neutrons in the space outside absorbing spheres or cylinders is stated analogously.
The solution of the Milne problem is conveniently given by applying the Laplace transform to the integro-differential transfer equation (see ) and using the Wiener–Hopf method to solve the functional equations thus obtained.
In order to solve the Milne problem it was suggested that expansion relative to generalized eigen functions and methods for solving singular integral equations be used (see ). The solution of the Milne problem for , is sought in the form
are the eigen functions of the continuous spectrum, denotes the Cauchy principal value, is the Dirac -function, and
The discrete eigen values are the roots of the characteristic equation
The eigen functions of the discrete spectrum take the form
The system of eigen functions and , , turns out to be complete in the space of generalized functions on the interval and they are orthogonal with respect to a weight which is the solution of a singular integral equation (see ).
The boundary condition (2) of the Milne problem gives :
that is, and are defined as the coefficients in the expansion of the function
The asymptotic density of the neutrons,
For , , the Hopf constant .
|||E.A. Milne, Mon. Notices Roy. Astron. Soc. , 81 (1921) pp. 361–375|
|||E. Hopf, "Mathematical problems of radiative equilibrium" , Cambridge Univ. Press (1934)|
|||I. Sneddon, "Fourier transforms" , McGraw-Hill (1951)|
|||K.M. Case, P.F. Zweifel, "Linear transport theory" , Addison-Wesley (1967)|
|[a1]||W. Greenberg, C. van der Mee, V. Protopopescu, "Boundary value problems in abstract kinetic theory" , Birkhäuser (1987)|
|[a2]||C. Cercignani, "The Boltzmann equation and its applications" , Springer (1988)|
|[a3]||B. Davison, J.B. Sykes, "Neutron transport theory" , Clarendon Press (1957)|
|[a4]||M.M.R. Williams, "The slowing down and thermalization of neutrons" , North-Holland (1966)|
Milne problem. V.A. Chuyanov (originator), Encyclopedia of Mathematics. URL: http://www.encyclopediaofmath.org/index.php?title=Milne_problem&oldid=17688