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The recently discovered new class of solar burst emission component exhibiting very fast pulses (durations approx 60 ms) at mm waves (lambda approx. mm) and at hard X-rays, poses serious constraints for interpretation assuming the acceleration of low energy electrons. An alternative interpretation is suggested assuming that the mm-wave emission component is part of a synchrotron radiation spectrum with peak emission in the infrared range of frequencies and accounting for fluxes reported for white-light flare emission in the visible range. Electron energies are reduced primarily by inverse Compton quenching on the synchrotron source photons, producing the observed X-rays and explaining the pulses' short time scales. According to this interpretation, the burst pulse sources must be very small (approx. 10 to the 6th power cm) with high brightness temperatures (approx. 10 the the 10th power 1 K). In a following step of the fast pulse, for t approx. 60 ms, the electrons energies decay to mildly relativistic or thermal energies, which may produce the better known longer lasting (t approx. 10 to the 6th power 60 ms) emissions at microwaves and X-rays.