SIMBAD references

We model the evolution of the water snowline in a protoplanetary disc from its birth to death. Since the disc forms from the collapse of the molecular cloud core, the core properties influence the snowline evolution. For the case of low angular momentum of the core, the disc is gravitationally stable. There is a unique snowline in the disc. It moves outward during the core collapse and then shrinks after the collapse ending. However, if the initial angular momentum of the cloud core is high, the disc is gravitationally unstable during the core collapse. Materials accumulates in the outer part of the low-viscosity region in the disc and the temperature of the disc in this region sharply increases. The snowline is pushed farther away from the central star in the core collapse stage. There is an inner icy region inside the snowline. After the core collapse ends, the snowline shrinks and the icy region disappear. Since icy materials in the inner icy region always exist during the disc lifetime, we suggest that the inner icy region may be the most favourable formation location of a giant planet. Finally, we discuss the implications of the disc dissipation by photoevaporation for terrestrial planet formation and the occurrence rate of debris discs.