Architectures of Planetary Systems II: Trends with Host Star Mass and Metallicity

TL;DR

This study analyzes how planetary system architectures relate to host star mass and metallicity, confirming some known trends and discovering new potential correlations, while noting that system architecture is generally independent of stellar properties.

Contribution

It extends previous classification frameworks to explore correlations with stellar mass and metallicity, revealing both confirmed and new trends in planetary system architectures.

Findings

Jovian planets are less common around low-mass, low-metallicity stars.

Total planetary mass increases with stellar mass.

Planetary system masses have an upper limit consistent with disk stability expectations.

Abstract

The current census of planetary systems displays a wide range of architectures. Extending earlier work, this paper investigates the correlation between our classification framework for these architectures and host stellar properties. Specifically, we explore how planetary system properties depend on stellar mass and stellar metallicity. This work confirms previously detected trends that jovian planets are less prevalent for low-mass and low-metallicity stars. We also find new, but expected trends such as that the total mass in planets increases with stellar mass, and that observed planetary system masses show an upper limit that is roughly consistent with expectations from the stability of circumstellar disks. We tentatively identify potential unique trends in the host stars of super-puffs and hot jupiters and a possible subdivision of the class of hot jupiter systems. In general, we find that system architectures are not overly dependent on host star properties.