A red giant branch common envelope evolution scenario for the exoplanet WD 1856 b

TL;DR

This paper proposes a new common envelope evolution scenario involving a red giant star engulfing a planet during its core helium flash, explaining the WD 1856+534 system with a planet orbiting a white dwarf.

Contribution

It introduces a novel energy deposition mechanism during the core helium flash that can lead to planetary engulfment and envelope ejection, expanding understanding of star-planet interactions.

Findings

Energy deposition reduces envelope binding energy.

Planet can unbind most of the envelope mass.

Scenario applicable to other white dwarf systems.

Abstract

We propose a common envelope evolution (CEE) scenario where a red giant branch (RGB) star engulfs a planet during its core helium flash to explain the puzzling system WD 1856+534 where a planet orbits a white dwarf (WD) of mass 0.52Mo with an orbital period of 1.4 day. At the heart of the scenario is the recently proposed assumption that the vigorous convection that core helium flash of RGB stars drive in the core excite waves that propagate and deposit their energy in the envelope. Using the binary-MESA stellar evolution code we show that this energy deposition substantially reduces the binding energy of the envelope and causes its expansion. We propose that in some cases RGB stars might engulf massive planets of ~0.01Mo during their core helium flash phase, and that the planet can unbind most of the mass of the bloated envelope. We show that there is a large range of initial orbital radii for which this scenario might take place under our assumptions. This scenario is relevant to other systems of close sub-stellar objects orbiting white dwarfs, like the brown dwarf-WD system ZTFJ003855.0+203025.5.