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Temperature changes in the planet forming disc midplanes carry importantphysico-chemical consequences, such as the effect on the locations of thecondensation fronts of molecules - the snowlines. Snowlines impose majorchemical gradients and possibly foster grain growth. The aim of this paper isto understand how disc midplane temperature changes with gas and dustevolution, and identify trends that may influence planet formation or allow toconstrain disc evolution observationally. We calculate disc temperature,hydrostatic equilibrium and dust settling in a mutually consistent way from agrid of disc models at different stages of gas loss, grain growth and holeopening. We find that the CO snowline location depends very strongly on discproperties. The CO snowline location migrates closer to the star for increasingdegrees of gas dispersal and dust growth. Around a typical A type star, thesnowline can be anywhere between several tens and a few hundred au, dependingon the disc properties such as gas mass and grain size. In fact, gas loss is asefficient as dust evolution in settling discs, and flat discs may be gas-poorcounterparts of flared discs. Our results, in the context of different pre-mainsequence evolution of the luminosity in low- and intermediate-mass starssuggests very different thermal (and hence chemical) histories in these twotypes of discs. Discs of T Tauri stars settle and cool down while discs ofHerbig Ae stars may remain rather warm throughout the pre-main sequence.

Effects of disc midplane evolution on CO snowline location