The future influence of six exoplanets on the envelope properties of their parent stars on the giant branches

TL;DR

This study models how six exoplanets influence their host stars' envelope properties during late stellar evolution, revealing potential for non-spherical mass loss and elliptical planetary nebula formation due to planetary spin-up and energy deposition.

Contribution

It provides the first detailed modeling of how specific exoplanets can significantly alter stellar envelope dynamics and shape planetary nebulae during the giant phases.

Findings

Massive exoplanets can spin up stellar envelopes to 10% of break-up velocity.

Planetary energy deposition can cause non-spherical mass loss and elliptical nebulae.

Most systems likely experience non-spherical mass loss due to planetary influence.

Abstract

We study the evolution of six exoplanetary systems with the stellar evolutionary code MESA and conclude that they will likely spin-up the envelope of their parent stars on the red giant branch (RGB) or later on the asymptotic giant branch (AGB) to the degree that the mass loss process might become non-spherical. We choose six observed exoplanetary systems where the semi-major axis is ~1-2AU, and use the binary mode of MESA to follow the evolution of the systems. In four systems the star engulfs the planet on the RGB, and in two systems on the AGB, and the systems enter a common envelope evolution (CEE). In two systems where the exoplanet masses are Mp~10MJ, where MJ is Jupiter mass, the planet spins-up the envelope to about 10% of the break-up velocity. Such envelopes are likely to have significant non-spherical mass loss geometry. In the other four systems where Mp~MJ the planet spins-up the envelope to values of ~1-2% of break-up velocity. Magnetic activity in the envelope that influences dust formation might lead to a small departure from spherical mass loss even in these cases. In the two cases of CEE on the AGB the planet deposits energy to the envelope that amounts to >10% of the envelope binding energy. We expect this to cause a non-spherical mass loss that will shape an elliptical planetary nebula in each case.