An upper limit on the ratio between the Extreme Ultraviolet and the bolometric luminosities of stars hosting habitable planets

TL;DR

This paper derives an upper limit on the ratio of EUV to bolometric luminosity in stars, which constrains the habitability of planets by limiting atmospheric mass loss driven by stellar radiation.

Contribution

It introduces a theoretical upper limit on stellar EUV to bolometric luminosity ratio, linking stellar radiation to planetary habitability constraints.

Findings

Many M-type stars likely cannot host habitable planets due to high EUV emissions.

The limit constrains atmospheric escape rates and planetary habitability.

Application to known stars suggests fewer habitable planets around M-type stars.

Abstract

A large number of terrestrial planets in the classical habitable zone of stars of different spectral types has already been discovered and many are expected to be discovered in near future. However, owing to the lack of knowledge on the atmospheric properties, the ambient environment of such planets are unknown. It is known that sufficient amount of Extreme Ultraviolet (EUV) radiation from the star can drive hydrodynamic outflow of hydrogen that may drag heavier species from the atmosphere of the planet. If the rate of mass loss is sufficiently high then substantial amount of volatiles would escape causing the planet to become uninhabitable. Considering energy-limited hydrodynamical mass loss with an escape rate that causes oxygen to escape alongwith hydrogen, I present an upper limit for the ratio between the EUV and the bolometric luminosities of stars which constrains the habitability of planets around them. Application of the limit to planet-hosting stars with known EUV luminosities implies that many M-type of stars should not have habitable planets around them.