Given a wave-length, these effects together determine combinations of pulse energy and duration which satisfy both limits. That solutions exist is shown by Fig. 2. This choice then fixes maximum system slant range z, once l and D b are picked. Note that the target effects lines move downward in proportion to the 4th power of D b . The present debris database cannot tell us the detailed composition of the 1 to 20-cm debris cloud.
Average power is, of course, inversely related to clearing time.
At this rate, a single detector operating only during the 3 hours of twilight can acquire the entire population in about 5 days. The variation of F with pulsewidth predicted by Eq. To take advantage of this possibility, we must find ablation data that justifies the use of this empirical equation, and redetermine the limiting factors posed by the Earth s atmosphere for propagating such short pulses. Recently, a flood of ablation data in the picosecond region has appeared. Ib, replacing SRS in that function, when picosecond pulses are substituted for 10-ns ones.