(Upper panel) The orbital energy distribution of the debris from a 1M _⊙ star disrupted after following an orbit with r _p ≃ 4.03r _g around an SMBH with M _BH = 10⁶ M _⊙. Energy is in units of Δϵ. The black dashed line shows the energy distribution in the gas remaining immediately after half the stellar mass plunges directly into the SMBH; the four colored curves show its evolution at later times. Here, E = −(1 + u _t) and ﹩{\rm{\Delta }}\epsilon ={{GM}}_{\mathrm{BH}}{R}_{\star }/{r}_{{\rm{t}}}^{2}﹩ where ﹩{r}_{{\rm{t}}}={({M}_{\mathrm{BH}}/{M}_{\star })}^{1/3}{R}_{\star }﹩. The time (in seconds) is measured since the initial pericenter passage. (Bottom panel) The thick black curve shows the mass fallback rate predicted from the energy distribution as of t = 40,000 s. The thin gray lines indicate the Eddington accretion rate assuming radiation efficiencies of η = 0.01 or 0.1.