Discovering the Growth Histories of Exoplanets: The Saturn Analog HD 149026b

TL;DR

This paper demonstrates that the large solid core of the exoplanet HD 149026b can be explained by standard core accretion theory, using a detailed model of its formation environment and migration history.

Contribution

It shows how to reconstruct the growth history of a planet with a well-defined core mass orbiting a solar-type star using a comprehensive formation model.

Findings

The planet's large core is consistent with core accretion theory.

Migration from 9.5 AU to 0.042 AU fits the formation scenario.

Heavy element enrichment influences disk solid mass requirements.

Abstract

The transiting "hot Saturn" HD 149026b, which has the highest mean density of any confirmed planet in the Neptune-Jupiter mass range, has challenged theories of planet formation since its discovery in 2005. Previous investigations could not explain the origin of the planet's 45-110 Earth-mass solid core without invoking catastrophes such as gas giant collisions or heavy planetesimal bombardment launched by neighboring planets. Here we show that HD 149026b's large core can be successfully explained by the standard core accretion theory of planet formation. The keys to our reconstruction of HD 149026b are (1) applying a model of the solar nebula to describe the protoplanet nursery; (2) placing the planet initially on a long-period orbit at Saturn's heliocentric distance of 9.5 AU; and (3) adjusting the solid mass in the HD 149026 disk to twice that of the solar nebula in accordance with the star's heavy element enrichment. We show that the planet's migration into its current orbit at 0.042 AU is consistent with our formation model. Our study of HD 149026b demonstrates that it is possible to discover the growth history of any planet with a well-defined core mass that orbits a solar-type star.