398 Prof. Schuster : Possible Effects of Solar Magnetization 



form. In fig. 2, E represents the pole of the ecliptic, P the 

 suit's axis of rotation, and M the magnetic axis. P and 

 E include an angle of 7°, and for practical purposes might 

 be taken to be coincident. If the sun is uniformly mag- 

 netized, we may treat the magnetic axis like a vector capable 



of projection. The original magnetization may then be con- 

 sidered as a superposition of magnetizations in three fixed 

 directions. We choose for these directions E, A, and B, 

 where the two latter lie in the ecliptic, A being the point of 

 intersection between that plane and a plane drawn through 

 P and E ; B is the sun's ascending node. The three 

 components of a unit vector M will be 



cos ME = cos 7 cos 8— sin 7 sin 8 cos xt, 

 sin ME cos MEP = sin 7 cos 8 cos Kt -f cos 7 sin 8 



= sin 7 cos Kt -f sin 8 cos 7 — i sin 2 - sin 7 cos Kt. 



and 



sin ME sin MEP= sin 7 sin Kt. 



In these equations 8 represents the angle between the sun's 

 equator and the ecliptic, 7 the angle between the axis of 

 rotation and the magnetic axis, and Kt the angle A P M, the 

 time here being reckoned from the instant that the magnetic 

 axis crosses the great circle P E, between P and A. 



It is seen that the magnetic effects of a rotating sphere of 

 unit moment may be considered to be made up of the super- 

 position of the following five systems : — 



(a) A fixed sphere permanently magnetized at right angles 

 to the ecliptic with moment cos 7 cos 8. The effect of such a 

 sphere has been discussed already by Lord Kelvin. If the 

 north-repelling pole is above the ecliptic, the result will be a 

 magnetic force parallel to the earth's axis acting from North 



CO 5 * 'V COS O COS € 



to South and equal to — 3 , and a force equal to 



