  We present a systematic analysis of type C quasi-periodic oscillation (QPO)
observations of H 1743--322 throughout the Rossi X-ray Timing Explorer (RXTE)
era. We find that, while different outbursts have significant flux differences,
they show consistent positive correlations between the QPO fractional
root-mean-square (rms) amplitude and non-thermal fraction of the emission,
which indicate an independence of the intrinsic QPO rms on individual outburst
brightness in H 1743--322. However, the dependence of the QPO rms on frequency
is different between the outburst rise and decay phases, where QPO fractional
rms of the decay phase is significantly lower than that of the rise phase at
low frequencies. The spectral analysis also reveals different ranges of coronal
temperature between the two outburst stages. A semi-quantitative analysis shows
that the Lense-Thirring precession model could be responsible for the QPO rms
differences, requiring a variable coronal geometric shape. However, the
variable-Comptonization model could also account for the findings. The fact
that the rms differences and the hysteresis traces in the hardness-intensity
diagram (HID) accompany each other indicates a connection between the two
phenomena. By correlating the findings with QPO phase lags and the
quasi-simultaneous radio flux previously published, we propose there could be
corona-jet transitions in H 1743--322 similar to those that have been recently
reported in GRS 1915+105.
