Solar-terrestrial time delays

Abstract

The observed delay of about 24 hours between the meridian passage of a sunspot or flare and the onset of an associated magnetic storm or aurora is shown to originate in the magnetic deflection of the ion streams involved. If a solar magnetic dipole is exclusively responsible, its moment must be between 6×1027 and 1029 gauss cm3. If an interplanetary magnetic field is involved, its magnitude is about 4×10−8 gauss. Should both fields act, which is likely, then the above figures represent maxima.

On an interplanetary magnetic field

“…However, the field of this dipole will cause a deflection in the proton beams even if the moment is quite small, thus contributing to the time lags or even being entirely responsible. for them [7]. Until the exact magnitude of the solar dipole moment is determined, the lags only provide an upper limit of 4 X 10 -s gauss to the interplanetary field near the sun.…”

“…A plausible argument can be made for equipartition, that is, that•Vs• = ,,v'/2 ........................... (s)at least on an average basis. On the other hand, from(7) we see that H increases more rapidly for the large wave-number (l/L) components of the turbulent fluid, which therefore preempt the supply of kinetic energy. Thus, H would vary wi• the size of the eddy.…”