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Gravitational lensing may render individual high-mass stars detectable out tocosmological distances, and several extremely magnified stars have in recentyears been detected out to redshifts $z\approx 6$. Here, we present Muspelheim,a model for the evolving spectral energy distributions of both metal-enrichedand metal-free stars at high redshifts. Using this model, we argue that lensedstars should form a highly biased sample of the intrinsic distribution of starsacross the Hertzsprung-Russell diagram, and that this bias will typically tendto favour the detection of lensed stars in evolved stages characterized by loweffective temperatures, even though stars only spend a minor fraction of theirlifetimes in such states. We also explore the prospects of detectingindividual, lensed metal-free (Population III) stars at high redshifts usingthe James Webb Space Telescope (JWST). We find that very massive ($\gtrsim 100\M_\odot$) Population III stars at $z\gtrsim 6$ may potentially be detected byJWST in surveys covering large numbers of strong lensing clusters, providedthat the Population III stellar initial mass function is sufficientlytop-heavy, that these stars evolve to effective temperatures $\leq 15000$ K,and that the cosmic star formation rate density of Pop III stars reaches$\gtrsim 10^{-4}\ M_\odot$ cMpc$^{-3}$ yr$^{-1}$ at $z\approx$ 6-10. Variousways to distinguish metal-free lensed stars from metal-enriched ones are alsodiscussed.

The detection and characterization of highly magnified stars with JWST: Prospects of finding Population III