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tokens: could be adjusted, but should not be orders of magnitude lower or the jet would not be observed in the EUV given the TRACE 195 Å response and reasonable temperatures. For the closed loop, the thermal density is taken to be cm −3 . Values larger than this would violate three observational constraints: (1) 195 Å emission would be stronger than observed for all reasonable coronal (including flaring) temperatures; (2) SXR emission would be stronger than is observed; and (3) the microwave spectrum would be dominated by a free–free component, which would not match the observed microwave spectral shape. The density could be smaller but would require adjustment of the loop geometry; therefore, there is a range of thermal densities that could fit the observed data. For the likely value of 1 × 10 10 cm −3 for the jet density, a temperature of 2.05 MK fits the measured TRACE 195 Å emission from the jet location. As the TRACE 195 Å temperature response function (Handy et al. 1999 ) decreases for all higher temperatures, a higher density would be required for any jet temperatures higher than this (and would violate the density constraint from microwave data mentioned earlier). For the closed loop, a density of cm −3 can produce the observed 195 Å brightness at the jet base, where this loop is located, for a temperature between 7.3 and 10.6 MK. Since the plasma temperature is not constrained within this range, we choose a temperature of 7.3 MK. For the nonthermal electrons in the jet, the microwave spectrum deviates from observations if the upper cutoff to the electron energy E max is below ∼300 keV; it is not well constrained from above. Further decrease of this parameter could be compensated by an increase of the source area, but this would be in conflict with the microwave source size. For the closed loop, the microwave spectrum deviates from observations if . In the model we use . 4. Discussion To recap the observations, we find high time variability in HXRs and microwaves, with HXR spectral hardening strongly correlated with fast bursts of intense flux. HXR images are dominated by the flaring (thermal) loops at low energies and (nonthermal) footpoints at high energies, but at intermediate energies (∼18–30 keV), some RHESSI emission is elongated along the jet, where OVSA data also reveal an elongated microwave source at the location of the jet. We interpret the fast HXR spikes as bursts of particle acceleration, and the duration of these peaks gives the timescale over which electrons are accelerated. The very short time lag between the burst intensity and its hardening (less than 200 ms in the case of G1 and no lag in the case of G2) implies that electrons are accelerated quickly to ∼100 keV. Combining the time lag from Figure 4 with the peak width from Figure 5 , we conclude that the event exhibits electron energy increases on an average timescale of 0.2 s, with acceleration episodes lasting, on average, 1 s. Once accelerated, the electrons that have