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We present analysis of two type-I X-ray bursts observed by NuSTAR originatingfrom the very faint transient neutron star low-mass X-ray binary GRS1741.9-2853 during a period of outburst in May 2020. We show that thepersistent emission can be modeled as an absorbed, Comptonized blackbody inaddition to Fe K$\alpha$ emission which can be attributed to relativistic diskreflection. We measure a persistent bolometric, unabsorbed luminosity of$L_{\mathrm{bol}}=7.03^{+0.04}_{-0.05}\times10^{36}\,\mathrm{erg\,s^{-1}}$,assuming a distance of 7 kpc, corresponding to an Eddington ratio of $4.5\%$.This persistent luminosity combined with light curve analysis leads us to inferthat the bursts were the result of pure He burning rather than mixed H/Heburning. Time-resolved spectroscopy reveals that the bolometric flux of thefirst burst exhibits a double-peaked structure, placing the source within asmall population of accreting neutron stars which exhibit multiple-peakedtype-I X-ray bursts. We find that the second, brighter burst shows evidence forphotospheric radius expansion (PRE) and that at its peak, this PRE event had anunabsorbed bolometric flux of$F_{\mathrm{peak}}=2.94^{+0.28}_{-0.26}\times10^{-8}\,\mathrm{erg\,cm^{-2}\,s^{-1}}$.This yields a new distance estimate of $d=9.0\pm0.5$ kpc, assuming that thiscorresponds to the Eddington limit for pure He burning on the surface of acanonical neutron star. Additionally, we performed a detailed timing analysiswhich failed to find evidence for quasiperiodic oscillations or burstoscillations, and we place an upper limit of $16\%$ on the rms variabilityaround 589 Hz, the frequency at which oscillations have previously beenreported.

Photospheric Radius Expansion and a double-peaked type-I X-ray burst from GRS 1741.9-2853