“bumps” observed in the lightcurve (see Fig. \[tics-02-08\]). The fast decay and the re-flares in the 2002 and 2005 show a similar duration. The 2008 outburst also shows comparable timescales, although with much higher uncertainty. As noted in § \[1Hz:intro\], in ’98 the observations stopped too early and the ’00 ones started too late to allow a similar comparison.

The precise determination of the re-flare periods suffers of biases due to occasional poor sampling and to the sensitivity limit of [[*RXTE*]{}]{}. Therefore, although the data certainly allow this, there is no significant evidence that differences in fast decay time scales between the 3 outbursts have an effect on the subsequent re-flare periodicity time scales.

In the 2008 outburst it is hard to calculate the re-flare time scale because the flux is below the sensitivity limit of [[*RXTE*]{}]{} in the majority of the observations. The [[*Swift*]{}]{} sampling was approximately 1 observation every 2 days, too long compared to the fast decay time scale of 3 days to unambiguously exclude shorter time scales. However, the fast decay and the re-flare time scales are again compatible with being the same.

In 2002 and 2005 the re-flares’ peak luminosity tends to decrease with time 