  Using black body and power-law photon counts of All Sky Monitor (ASM) in
Rossi X-ray Timing Explorer (RXTE) satellite it has been established recently
by us that there is a significant time lag between the infall timescales of two
components in the Two-Component Advective Flow (TCAF) paradigm, where a
standard slow moving Keplerian disc is surrounded by a fast moving halo. The
time lag is clearly due to the difference in viscosity in the flow components
and the size of the Keplerian disc may be considered to be proportional to the
arrival time lag. In this paper, using RXTE/ASM (1.5-12 keV) data, we examine
eight successive outbursts of the low-mass X-ray binary H 1743-322 since 2003
from a new angle. A dynamic photon index, {\Theta} indicates that the size of
the Keplerian disc is biggest during the brightest outburst of 2003. The size
diminishes thereafter during subsequent weaker outbursts. These results are
corroborated when two energy fluxes corresponding to the two flows are
cross-correlated with reference to {\Theta}. Moreover, {\Theta} decides
spectral transitions of any outburst. We show from the behaviour of {\Theta}
alone that the outburst of October 2008 was an anomalous outburst. In fact,
each normal outburst was either preceded or followed by an otherwise premature
outburst. This makes H 1743-322 an enigmatic source and a subject of further
study.
