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In this paper, the third in this series, we continue our study of tidaldisruption events of main-sequence stars by a non-spinning$10^{6}~\rm{M}_\odot$ supermassive black hole. Here we focus on the stellarmass dependence of the outcomes of partial disruptions. As the encounterbecomes weaker, the debris mass is increasingly concentrated near the outeredges of the energy distribution. As a result, the mass fallback rate candeviate substantially from a $t^{-5/3}$ power-law, becoming more like a singlepeak with a tail declining as $t^{-p}$ with $p\simeq2-5$. Surviving remnantsare spun-up in the prograde direction and are hotter than main sequence starsof the same mass. Their specific orbital energy is $\simeq10^{-3}\times$ thatof the debris, but of either sign with respect to the black hole potential,while their specific angular momentum is close to that of the original star.Even for strong encounters, remnants have speeds at infinity relative to theblack hole potential $\lesssim 300$ km s$^{-1}$, so they are unable to travelfar out into the galactic bulge. The remnants most deeply bound to the blackhole go through a second tidal disruption event upon their first return topericenter; if they have not thermally relaxed, they will be completelydisrupted.

Tidal disruptions of main sequence stars -- III. Stellar mass dependence of the character of partial disruptions