The stellar birth environment can significantly shorten protoplanetary disc ( PPD ) lifetimes due to the influence of stellar feedback mechanisms .
The degree to which these mechanisms suppress the time and mass available for planet formation is dependent on the local far-ultraviolet ( FUV ) field strength , stellar density , and ISM properties .
In this work , we present the first theoretical framework quantifying the distribution of PPD dispersal time-scales as a function of parameters that describe the galactic environment .
We calculate the probability density function for FUV flux and stellar density in the solar neighbourhood .
In agreement with previous studies , we find that external photoevaporation is the dominant environment-related factor influencing local stellar populations after the embedded phase .
Applying our general prescription to the Central Molecular Zone of the Milky Way ( i.e .
the central \sim 250 ~ { } \mbox { $ { pc } $ } ) , we predict that 90 \% of PPDs in the region are destroyed within 1 Myr of the dispersal of the parent molecular cloud .
Even in such dense environments , we find that external photoevaporation is the dominant disc depletion mechanism over dynamical encounters between stars .
PPDs around low-mass stars are particularly sensitive to FUV-induced mass loss , due to a shallower gravitational potential .
For stars of mass \sim 1 ~ { } \mbox { M$ { } _ { \odot } $ } , the solar neighbourhood lies at approximately the highest gas surface density for which PPD dispersal is still relatively unaffected by external FUV photons , with a median PPD dispersal timescale of \sim 4 Myr .
We highlight the key questions to be addressed to further contextualise the significance of the local galactic environment for planet formation .