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In this Letter we discuss what happens to hydrogen recombination energy thatis released during regular common envelope (CE) events, as opposed toself-regulated CE events. We show that the amount of recombination energy thatcan be transferred away by either convection or radiation from the regionswhere recombination takes place is negligible. Instead, recombination energy isdestined to be used either to help CE expansion, as a work term, or toaccelerate local fluid elements. The exceptions are donors that initially havevery high entropy material, $S/(k_B N_A)>37$ mol g$^{-1}$. The analysis andconclusions are independent of specific stellar models or evolutionary codes,and rely on fundamental properties of stellar matter such as the equation ofstate, Saha equation and opacities, as well as on stellar structure equationsand the mixing length theory of convection.

On the use of hydrogen recombination energy during common envelope events