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Low and intermediate mass stars lose a significant fraction of their massthrough a dust-driven wind during the Asymptotic Giant Branch (AGB) phase.Recent studies show that winds from late-type stars are far from being smooth.Mass-loss variations occur on different time scales, from years to tens ofthousands of years. The variations appear to be particularly prominent towardsthe end of the AGB evolution. The occurrence, amplitude and time scale of thesevariations are still not well understood.  The goal of our study is to gain insight into the structure of thecircumstellar envelope (CSE) of WX Psc and map the possible variability of thelate-AGB mass-loss phenomenon.  We have performed an in-depth analysis of the extreme infrared AGB star WXPsc by modeling (1) the CO J=1-0 through 7-6 rotational line profiles and thefull spectral energy distribution (SED) ranging from 0.7 to 1300 micron. Wehence are able to trace a geometrically extended region of the CSE.  Both mass-loss diagnostics bear evidence of the occurrence of mass-lossmodulations during the last ~2000 yr. In particular, WX Psc went through a highmass-loss phase (Mdot~5e-5 Msun/yr) some 800 yr ago. This phase lasted about600 yr and was followed by a long period of low mass loss (Mdot~5e-8 Msun/yr).The present day mass-loss rate is estimated to be ~6e-6 Msun/yr.  The AGB star WX Psc has undergone strong mass-loss rate variability on a timescale of several hundred years during the last few thousand years. Thesevariations are traced in the strength and profile of the CO rotational linesand in the SED. We have consistently simulated the behaviour of both tracersusing radiative transfer codes that allow for non-constant mass-loss rates.

The variable mass loss of the AGB star WX Psc as traced by the CO J=1-0 through 7-6 lines and the dust emission