On the use of hydrogen recombination energy during common envelope events

Abstract

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

7 pages, 5 figures, ApJL accepted

References in corpus (5)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Recombination energy in double white dwarf formation
• Common envelope events with low-mass giants: understanding the transition to the slow spiral-in
• The limited role of recombination energy in common envelope removal
• Energy transport by convection in the common envelope evolution

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