Using a common methodology to analyze data from the AMPTE/IRM and ISEE 2 satellites we report on the statistical properties of bursty bulk flow events (BBFs) in the inner plasma sheet (IPS). A positive correlation between BBFs and the AE index suggests that BBFs are predominantly geomagnetically active time phenomena. Earthward BBFs are more frequent close to midnight and away from Earth, up to a distance of ~19 RE. Tailward BBFs are very infrequent in the IRM data set and somewhat less infrequent in the ISEE 2 data set in the region of the satellites' spatial overlap, possibly due to the more active conditions prevailing during the ISEE 2 mission in that region. However, in both data sets the ratio of tailward to earthward BBFs increases with distance from Earth; more than 20% of all BBFs are anti-sunward tailward of X = -19 RE in the ISEE 2 data set. BBFs are responsible for 60-100% of the measured earthward transport of mass, energy and magnetic flux past the satellite in the regions of maximum occurrence rate, even though they last approximately 10-15% of the IPS observation time there. Thus BBFs represent the primary transport mechanism at those regions. The one-to-one correspondence between BBFs and substorm phase, as well as the relative contribution of BBFs to the total transport observed during substorms are questions that await further investigation based on multi instrument studies of individual events. vicinity of the neutral sheet was found to be quite dynamic in the AMPTE/IRM data set, contrary to conclusions based primarily on data from the ISEE satellites [Eastman et al., 1985]. In addition, the direction of the bursts of plasma flow in the ICPS is predominantly across the instantaneous magnetic field, rendering them possible significant contributors to the total measured magnetic flux transport. The high speed flows in the ICPS were studied on a case-bycase basis by Angelopoulos et al. [1992a]. The authors concluded that the rise-and-fall timescale of the flow bursts is of the order of a minute and that the bursts occur within 10-rain timescale flow enhancements termed bursty bulk flow events (BBFs). The bursts of flow are associated with ion heating and plasma sheet dipolarization. In a statistical study of BBFs in the AMPTE/IRM data set, Angelopoulos et al. [ 1992b] showed that such events are relatively infrequent (< 7% of the time in the plasma sheet and < 20% of the time in the ICPS) but can produce roughly half of the earthward mass and energy transport measured past the satellite during its 1985 magnetotail passes and most of the earthward magnetic flux transport. Thus such events represent important building blocks of magnetotail transport. High speed flows in the near-Earth central plasma sheet (CPS) have been reported in the past, in particular in data from the ISEE satellites [e.g., Hones, 1979; Nishida et al., 1981; Cattell and Mozer, 1984; Huang et al., 1987; Ohtani et al., 1992; Sergeev et al., 1992]. However, such flows have received little attention from the point of view of trans...

[1] We present evidence based on measurements from the Polar spacecraft for the existence of small-scale, large-amplitude kinetic Alfvén waves/spikes at the plasma sheet boundary layer (PSBL) at altitudes of 4-6 R E . These structures coincide with larger-scale Alfvénic waves that carry a large net Poynting flux along magnetic field lines toward the Earth. Both structures are typically observed in the PSBL but have also been observed deeper in the plasma sheet. The small-scale spikes have electric field amplitudes up to 300 mV m À1 and associated magnetic field variations between 0.5 and 5 nT. Previous analysis has shown that the larger-scale Alfvén waves have periods of $20-60 s and carry enough Poynting flux to explain the generation of the most intense auroral structures observed in the Polar Ultraviolet Imager data set. In this paper it is shown that the smaller-scale waves have durations in the spacecraft frame of 250 ms to 1 s (but may have shorter time durations since the Nyquist frequency of the magnetic field experiment is $4 Hz.). The characteristic ratio of the amplitudes of the electric to magnetic field fluctuations is strong evidence that the waves are kinetic Alfvén waves with scale sizes perpendicular to the magnetic field on the order of 20-120 km (with an electron inertial length c/w pe $10 km and an ion gyroradius $20 km). Theoretical analysis of the observed spikes suggests that these waves should be very efficient at accelerating electrons parallel to the magnetic field. Simultaneously measured electron velocity space distribution functions from the Polar Hydra instrument include parallel electron heating features and earthward electron beams, indicating strong parallel energization. The characteristic parallel energy is on the order of $1 keV, consistent with estimates of the parallel R Edl associated with small-scale kinetic Alfvén wave structures. The energy flux in the electron ''beams'' is $0.7 ergs cm À2 s À1 . These observations suggest that the small-scale kinetic Alfvén waves are generated from the larger-scale Alfvén waves through one or more of a variety of mechanisms that have been proposed to result in the filamentation of large-amplitude Alfvén waves. The observations presented herein provide strong evidence that in addition to the auroral particle energization processes known to occur at altitudes between 0.5 and 2 R E , there are important heating and acceleration mechanisms operating at these higher altitudes in the plasma sheet.

The contribution to the total energy flux at these altitudes from Poynting flux associated with Alfven waves is comparable to or larger than the contribution from the particle energy flux and 1-2 orders of magnitude larger than that estimated from the large-scale steady state convection electric field and field-aligned current system.

The typically dark surface of the dwarf planet Ceres is punctuated by areas of much higher albedo, most prominently in the Occator crater. These small bright areas have been tentatively interpreted as containing a large amount of hydrated magnesium sulfate, in contrast to the average surface, which is a mixture of low-albedo materials and magnesium phyllosilicates, ammoniated phyllosilicates and carbonates. Here we report high spatial and spectral resolution near-infrared observations of the bright areas in the Occator crater on Ceres. Spectra of these bright areas are consistent with a large amount of sodium carbonate, constituting the most concentrated known extraterrestrial occurrence of carbonate on kilometre-wide scales in the Solar System. The carbonates are mixed with a dark component and small amounts of phyllosilicates, as well as ammonium carbonate or ammonium chloride. Some of these compounds have also been detected in the plume of Saturn’s sixth-largest moon Enceladus. The compounds are endogenous and we propose that they are the solid residue of crystallization of brines and entrained altered solids that reached the surface from below. The heat source may have been transient (triggered by impact heating). Alternatively, internal temperatures may be above the eutectic temperature of subsurface brines, in which case fluids may exist at depth on Ceres today.