Consider the Proca equations for a localized steady-state distribution of current that has only a static magnetic moment. This model can be used to study the observable effects of a finite photon mass on the earth's magnetic field. Note that if the magnetization is M(x) the current density can be written as J=c(∇×M).
(a) Show that if M=mf(x), where m is a fixed vector and f(x) is a localized scalar function, the vector potential is
A(x)=−m×∇∫f(x′)∣x−x′∣e−μ∣x−x′∣d3x′
(b) If the magnetic dipole is a point dipole at the origin [f(x)=δ(x)], show that the magnetic field away from the origin is
B(x)=[3r^(r^⋅m)−m](1+μr+3μ2r2)r3e−μr−32μ2mre−μr
(c) The result of part b shows that at fixed r=R (on the surface of the earth), the earth's magnetic field will appear as a dipole angular distribution, plus an added constant magnetic field (an apparently external field) antiparallel to m. Satellite and surface observations lead to the conclusion that this ``external'' field is less than 4×10−3 times the dipole field at the magnetic equator. Estimate a lower limit on μ−1 in earth radii and an upper limit on the photon mass in grams from this datum.
This method of estimating μ is due to E. Schr\"odinger, Proc. R. Irish Acad. A49, 135 (1943). See A. S. Goldhaber and M. M. Nieto, Phys. Rev. Lett. 21, 567 (1968).