  We present stellar evolution calculations from the Asymptotic Giant Branch
(AGB) to the Planetary Nebula (PN) phase for models of initial mass 1.2 M\odot
and 2.0 M\odot that experience a Late Thermal Pulse (LTP), a helium shell flash
that occurs following the AGB and causes a rapid looping evolution between the
AGB and PN phase. We use these models to make comparisons to the central star
of the Stingray Nebula, V839 Ara (SAO 244567). The central star has been
observed to be rapidly evolving (heating) over the last 50 to 60 years and
rapidly dimming over the past 20 - 30 years. It has been reported to belong to
the youngest known planetary nebula, now rapidly fading in brightness. In this
paper we show that the observed timescales, sudden dimming, and increasing
Log(g), can all be explained by LTP models of a specific variety. We provide a
possible explanation for the nebular ionization, the 1980s sudden mass loss
episode, the sudden decline in mass loss, and the nebular recombination and
fading.
