We have evaluated the energetics of 38 solar eruptive events observed by a variety of spacecraft instruments between February 2002 and December 2006, as accurately as the observations allow. The measured energetic components include: (1) the radiated energy in the GOES 1 -8Å band; (2) the total energy radiated from the soft X-ray (SXR) emitting plasma; (3) the peak energy in the SXR-emitting plasma; (4) the bolometric radiated energy over the full duration of the event; (5) the energy in flare-accelerated electrons above 20 keV and in flareaccelerated ions above 1 MeV; (6) the kinetic and potential energies of the coronal mass ejection (CME); (7) the energy in solar energetic particles (SEPs) observed in interplanetary space; and (8) the amount of free (nonpotential) magnetic energy estimated to be available in the pertinent active region. Major conclusions include: (1) the energy radiated by the SXR-emitting plasma exceeds, by about half an order of magnitude, the peak energy content of the thermal plasma that produces this radiation; (2) the energy content in flare-accelerated electrons and ions is sufficient to supply the bolometric energy radiated across all wavelengths throughout the event; (3) the energy contents of flare-accelerated electrons and ions are comparable; (4) the energy in SEPs is typically a few percent of the -2 -CME kinetic energy (measured in the rest frame of the solar wind); and (5) the available magnetic energy is sufficient to power the CME, the flare-accelerated particles, and the hot thermal plasma.Subject headings: Sun: activity -Sun: coronal mass ejections -Sun: flares -Sun: particle emission -Sun: X-rays, gamma rays * In yy/mm/dd format. * * GOES start time (UT). 1 Radiated energy in the GOES 1 -8Å band. 2 Total radiated energy from the SXR-emitting plasma. 3 Bolometric radiated energy. 4 Peak thermal energy of the SXR-emitting plasma. 5 Energy in flare-accelerated electrons. 6 Energy in flare-accelerated ions. 7 CME kinetic energy in the rest frame of the Sun. 8 CME kinetic energy in solar-wind rest frame. 9 CME gravitational potential energy. 10 Energy in SEPs. 11 Nonpotential magnetic energy in the active region.† Behind-the-limb event. ‡Bolometric irradiance directly measured with TIM -see Table 2.

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[1] During a passage through the Earth's dawn-side outer radiation belt, whistler-mode waves with amplitudes up to more than $240 mV/m were observed by the STEREO S/WAVES instrument. These waves are an order of magnitude larger than previously observed for whistlers in the radiation belt. Although the peak frequency is similar to whistler chorus, there are distinct differences from chorus, in addition to the larger amplitudes, including the lack of drift in frequency and the oblique propagation with a large longitudinal electric field component. Simulations show that these large amplitude waves can energize an electron by the order of an MeV in less than 0.1s, explaining the rapid enhancement in electron intensities observed between the STEREO-B and STEREO-A passage during this event. Our results show that the usual theoretical models of electron energization and scattering via small-amplitude waves, with timescales of hours to days, may be inadequate for understanding radiation belt dynamics. Citation: Cattell, C., et al. (2008), Discovery of very large amplitude whistler-mode waves in Earth's radiation belts, Geophys. Res. Lett., 35, L01105,