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Recently, several accreting M dwarf stars have been discovered with ages farexceeding the typical protoplanetary disc lifetime. These `Peter Pan discs' canbe explained as primordial discs that evolve in a low-radiation environment.The persistently low masses of the host stars raise the question whetherprimordial discs can survive up to these ages around stars of higher mass. Inthis work we explore the way in which different mass loss processes inprotoplanetary discs limit their maximum lifetimes, and how this depends onhost star mass. We find that stars with masses $\lesssim$ 0.6 M$_\odot$ canretain primordial discs for $\sim$50 Myr. At stellar masses $\gtrsim$ 0.8M$_\odot$, the maximum disc lifetime decreases strongly to below 50 Myr due torelatively more efficient accretion and photoevaporation by the host star.Lifetimes up to 15 Myr are still possible for all host star masses up to$\sim$2 M$_\odot$. For host star masses between 0.6 and 0.8 M$_\odot$,accretion ceases and an inner gap forms before 50 Myr in our models.Observations suggest that such a configuration is rapidly dispersed. Weconclude that Peter Pan discs can only occur around M dwarf stars.

Exploring the possibility of Peter Pan discs across stellar mass