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We use a simple framework to calculate the time evolution of the compositionof the fallback material onto a supermassive black hole arising from the tidaldisruption of main sequence stars. We study stars with masses between 0.8 and3.0 $M_\odot$, at evolutionary stages from zero-age main sequence toterminal-age main sequence, built using the Modules for Experiments in StellarAstrophysics code. We show that most stars develop enhancements in nitrogen($^{14}$N) and depletions in carbon ($^{12}$C) and oxygen ($^{16}$O) over theirlifetimes, and that these features are more pronounced for higher mass stars.We find that, in an accretion-powered tidal disruption flare, these featuresbecome prominent only after the time of peak of the fallback rate and appear atearlier times for stars of increasing mass. We postulate that no severecompositional changes resulting from the fallback material should be expectednear peak for a wide range of stellar masses and, as such, are unable toexplain the extreme helium-to-hydrogen line ratios observed in some TDEs. Onthe other hand, the resulting compositional changes could help explain thepresence of nitrogen-rich features, which are currently only detected afterpeak. When combined with the shape of the light curve, the time evolution ofthe composition of the fallback material provides a clear method to helpconstrain the nature of the disrupted star. This will enable a bettercharacterization of the event by helping break the degeneracy between the massof the star and the mass of the black hole when fitting tidal disruption lightcurves.

Tidal Disruptions of Main Sequence Stars of Varying Mass and Age: Inferences from the Composition of the Fallback Material