CHARACTERISTICS OF MAGNETIC FLUCTUATIONS WITHIN CORONAL MASS EJECTIONS - THE JANUARY 1997 EVENT

We determine the geometry of the fluctuations of the magnetic field at frequencies just above the proton gyrofrequency for the January 10, 1 997 CME and the magnetic cloud within. The transverse magnetic fluctua tions represent a greater fraction of the magnetic energy than is the case in the typical undisturbed solar wind. The break in the power spe ctrum that is associated with the the onset of magnetic dissipation fa lls within the frequency range of interest. The fluctuation geometry i s markedly different above and below the spectral break frequency. The inertial range geometry remains unchanged in the cloud with only simi lar to 30% of the energy associated with field-aligned wave vectors. T he dissipation range wave vectors are highly oblique to the mean magne tic field B with up to 96% of the energy associated with oblique wave vectors.