We present the weak lensing mass calibration of the stellar mass based $mu_{star}$ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time we are able to perform a calibration of $mu_{star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 leqslant z<0.65$ and $mu_{star}$ up to $sim 5.5 times 10^{13} M_{odot}$, and infer the average masses of these subsets through modelling of their stacked weak lensing signal. In our model we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, cluster-member contamination of the source sample, deviations from the NFW halo profile, halo triaxiality and projection effects. We use the inferred masses to estimate the joint mass--$mu_{star}$--$z$ scaling relation given by $langle M_{200c} | mu_{star},z rangle = M_0 (mu_{star}/5.16times 10^{12} mathrm{M_{odot}})^{F_{mu_{star}}} ((1+z)/1.35)^{G_z}$. We find $M_0= (1.14 pm 0.07) times 10^{14} mathrm{M_{odot}}$ with $F_{mu_{star}}= 0.76 pm 0.06$ and $G_z= -1.14 pm 0.37$. We discuss the use of $mu_{star}$ as a complementary mass proxy to the well-studied richness $lambda$ for: $i)$ exploring the regimes of low $z$, $lambda<20$ and high $lambda$, $z sim 1$; $ii)$ testing systematics such as projection effects for applications in cluster cosmology.
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