Habitable Zone Boundaries for Circumbinary Planets

TL;DR

This study estimates habitable zone boundaries for terrestrial planets around various circumbinary star systems using a 1-D climate model, revealing how planetary mass and stellar types influence habitable zones.

Contribution

It provides the first systematic analysis of habitable zone boundaries for planets around diverse binary star systems considering planetary mass effects.

Findings

Inner edge of HZ moves inward for larger planets across all stellar types.

Outer edge of HZ remains relatively unchanged despite planetary mass.

Identifies a common stellar flux domain for habitable zones in circumbinary systems.

Abstract

We use a one-dimensional (1-D) cloud-free climate model to estimate habitable zone (HZ) boundaries for terrestrial planets of masses 0.1 M$_{E}$ and 5 M$_{E}$ around circumbinary stars of various spectral type combinations. Specifically, we consider binary systems with host spectral types F-F, F-G, F-K, F-M, G-G, G-K, G-M, K-K, K-M and M-M. Scaling the background N2 atmospheric pressure with the radius of the planet, we find that the inner edge of the HZ moves inwards towards the star for 5ME compared to 0.1ME planets for all spectral types. This is because the water-vapor column depth is smaller for larger planets and higher temperatures are needed before water vapor completely dominates the outgoing longwave radiation. The outer edge of the HZ changes little due to competing effects of the albedo and greenhouse effect. While these results are broadly consistent with the trend of single star HZ results for different mass planets, there are significant differences between single star and binary star systems for the inner edge of the HZ. Interesting combinations of stellar pairs from our 1-D model results can be used to explore for in-depth climate studies with 3-D climate models. We identify a common HZ stellar flux domain for all circumbinary spectral types