Planetary nebulae after common-envelope phases initiated by low-mass red giants

TL;DR

This paper investigates the conditions under which planetary nebulae form after common-envelope phases initiated by low-mass red giants, focusing on the remnant structures and their evolution to produce observable nebulae.

Contribution

It introduces a model for post-CE remnant structures based on core mass and envelope properties, predicting planetary nebula formation conditions.

Findings

Planetary nebulae form if the remnant's core exceeds ~0.3 solar masses.

Remnants in thermal equilibrium are more likely to produce planetary nebulae.

The presence of a pre-white dwarf plateau depends on the envelope mass at CE end.

Abstract

It is likely that at least some planetary nebulae are composed of matter which was ejected from a binary star system during common-envelope (CE) evolution. For these planetary nebulae the ionizing component is the hot and luminous remnant of a giant which had its envelope ejected by a companion in the process of spiralling-in to its current short-period orbit. A large fraction of CE phases which end with ejection of the envelope are thought to be initiated by low-mass red giants, giants with inert, degenerate helium cores. We discuss the possible end-of-CE structures of such stars and their subsequent evolution to investigate for which structures planetary nebulae are formed. We assume that a planetary nebula forms if the remnant reaches an effective temperature greater than 30 kK within 10^4 yr of ejecting its envelope. We assume that the composition profile is unchanged during the CE phase so that possible remnant structures are parametrized by the end-of-CE core mass, envelope mass and entropy profile. We find that planetary nebulae are expected in post-CE systems with core masses greater than about 0.3 solar masses if remnants end the CE phase in thermal equilibrium. We show that whether the remnant undergoes a pre-white dwarf plateau phase depends on the prescribed end-of-CE envelope mass. Thus, observing a young post-CE system would constrain the end-of CE envelope mass and post-CE evolution.