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Far-IR 16-1000 $\mu$m spectra of Saturn's hydrogen-helium continuum measuredby Cassini's Composite Infrared Spectrometer (CIRS) are inverted to construct anear-continuous record of upper tropospheric (70-700 mbar) temperatures andpara-H$_2$ fraction as a function of latitude, pressure and time for a third ofa Saturnian year (2004-2014, from northern winter to northern spring). Thethermal field reveals evidence of reversing summertime asymmetries superimposedonto the belt/zone structure. The temperature structure that is almostsymmetric about the equator by 2014, with seasonal lag times that increase withdepth and are qualitatively consistent with radiative climate models. Localisedheating of the tropospheric hazes (100-250 mbar) create a distinct perturbationto the temperature profile that shifts in magnitude and location, declining inthe autumn hemisphere and growing in the spring. Changes in the para-H$_2$($f_p$) distribution are subtle, with a 0.02-0.03 rise over the springhemisphere (200-500 mbar) perturbed by (i) low-$f_p$ air advected by both thespringtime storm of 2010 and equatorial upwelling; and (ii) subsidence ofhigh-$f_p$ air at northern high latitudes, responsible for a developingnorth-south asymmetry in $f_p$. Conversely, the shifting asymmetry in thepara-H$_2$ disequilibrium primarily reflects the changing temperature structure(and the equilibrium distribution of $f_p$), rather than actual changes in$f_p$ induced by chemical conversion or transport. CIRS results interpolated tothe same point in the seasonal cycle as re-analysed Voyager-1 observations showqualitative consistency, with the exception of the tropical tropopause near theequatorial zones and belts, where downward propagation of a cool temperatureanomaly associated with Saturn's stratospheric oscillation could potentiallyperturb tropopause temperatures, para-H$_2$ and winds. [ABRIDGED]

Seasonal Variability of Saturn's Tropospheric Temperatures, Winds and Para-H$_2$ from Cassini Far-IR Spectroscopy