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This study presents a 13 years survey of haze UV extinction profiles,monitoring the temporal evolution of the detached haze layer (DHL) in Titan'supper atmosphere (350-600 km). As reported by West et al. 2011 (GRL vol.38,L06204) at the equator, we show that the DHL is present at all latitudes below55{\deg}N during the northern winter (2004-2009). Then, it globally sunk anddisappeared in 2012. No permanent DHL was observed between 2012 and 2015. It'sonly in late-2015, that a new structure emerged from the Northern hemisphereand propagated to the equator. This new DHL is not as pronounced as in 2004 andis much more complex than the one observed earlier. In one specific sequence,in 2005, we were able to investigate the short time scale variability of theDHL and no major changes was observed. When both side of the limb were visible(dawn/dusk), we notice that the extinction of the DHL is slightly higher on thedawn side. Additionally, during a polar flyby in 2009, we observed thelongitudinal variability of the DHL and spotted some local inhomogeneities.Finally, comparisons with UVIS stellar occultations and General Climate Models(GCMs) are both consistent with our findings. However, we noticed that thetiming of the DHL main pattern predicted by the GMCs can be off by up to30{\deg} in solar longitude. All these observations bring new perspectives onthe seasonal cycle of Titan's upper atmosphere, the evolution of the DHL andits interaction with the dynamics.

Haze seasonal variations of Titan's upper atmosphere during the Cassini Mission