  Rotating radio transients (RRATs), loosely defined as objects that are
discovered through only their single pulses, are sporadic pulsars that have a
wide range of emission properties. For many of them, we must measure their
periods and determine timing solutions relying on the timing of their
individual pulses, while some of the less sporadic RRATs can be timed by using
folding techniques as we do for other pulsars. Here, based on Parkes and Green
Bank Telescope (GBT) observations, we introduce our results on eight RRATs
including their timing-derived rotation parameters, positions, and dispersion
measures (DMs), along with a comparison of the spin-down properties of RRATs
and normal pulsars. Using data for 24 RRATs, we find that their period
derivatives are generally larger than those of normal pulsars, independent of
any intrinsic correlation with period, indicating that RRATs' highly sporadic
emission may be associated with intrinsically larger magnetic fields. We carry
out Lomb$-$Scargle tests to search for periodicities in RRATs' pulse detection
times with long timescales. Periodicities are detected for all targets, with
significant candidates of roughly 3.4 hr for PSR J1623$-$0841 and 0.7 hr for
PSR J1839$-$0141. We also analyze their single-pulse amplitude distributions,
finding that log-normal distributions provide the best fits, as is the case for
most pulsars. However, several RRATs exhibit power-law tails, as seen for
pulsars emitting giant pulses. This, along with consideration of the selection
effects against the detection of weak pulses, imply that RRAT pulses generally
represent the tail of a normal intensity distribution.

High Energy Astrophysical Phenomena;Instrumentation and Methods for Astrophysics