Evolution of important powers associated with the He-rich shell in our sample of He-star explosion models. Top: Fractional line flux in [N II] λλ 6548, 6583 relative to the total optical luminosity versus time since explosion for our radiative-transfer calculations based on the ejecta models he2p6 to he12p0 arising from He-star progenitors evolved with the nominal mass loss rate (Woosley 2019; Ertl et al. 2020, solid line) and on the ejecta models he2p5MdZ to he4p5MdZ arising from He-star progenitors evolved with no mass loss (dashed line). Bottom: Same as above but showing the fraction of the total decay power absorbed in the He-rich shell. Both are given as a percentage.