  We review the longterm confusion which has existed over the nature of flaring
in the brightest class of low mass X-ray binary: the Z-track sources,
specifically in the Cygnus X-2 sub-group. Intensity reductions in the
lightcurve produce a branch in colour -colour diagrams similar to that of real
flares in the Sco X-1 like group, and the nature of this branch was not clear.
However, based on observations of Cygnus X-2 in which this dipping/flaring
occurred it was proposed that the mass accretion rate in Z-track sources in
general increases monotonically along the Z-track towards the Flaring Branch, a
standard assumption widely held. It was also suggested that the Cygnus X-2
group have high inclination. Based on recent multi-wavelength observations of
Cygnus X-2 we resolve these issues, showing by spectral analysis that the
Dipping Branch consists of absorption events in the outer disk, unrelated to
the occasional real flaring in the source. Thus motivation for Mdot increasing
along the Z from Horizontal - Normal to Flaring Branch is removed, as is the
idea that high inclination distinguishes the Cygnus X-2 group. Finally, the
observations provide further evidence for the extended nature of the Accretion
Disk Corona (ADC), and the correct modelling of the ADC Comptonized emission is
crucial to the interpretation of low mass X-ray binary data.
