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Fall times down to 1.5 ns have been measured.
The pulse rise and fall times were varied between 0.1 and 10 ps in different simulations.
During the period, both rise and fall times are 10 −7 s.
A minimum width of 20 ns is possible and the rise and fall times are typically 5 and 7 ns.
Furthermore, this will improve the transient characteristics by reducing the rise and fall times and makes dynamic performance better.
Moreover, the extremely fast rise and fall times of 33 µs and 30 µs were achieved without any external bias application.
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If necessary, some of the equipment can be turned off during the long free-fall times.
Ground-based experiments addressing these questions may soon face limitations due to limited free-fall times and the quality of vacuum and microgravity.
This approach does not only NOT require extreme UV light, it also brings the benefit of much shorter free-fall times and higher interference visibilities.
This allows sufficiently suppressing quantum decoherence for the effects of alternative theoretical models to become experimentally accessible, and to observe the evolution of macroscopic superpositions over free-fall times of about 100 s.
Due to the Courant constraint, it is not possible to model the accretion phase accurately for more than a few free-fall times, or ({simeq}10mbox { yr}) (Ripamonti et al. 2002; Greif et al. 2012).
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