The dispersal of protoplanetary discs -- III: Influence of stellar mass on disc photoevaporation

TL;DR

This study investigates how stellar mass influences disc dispersal via X-ray photoevaporation, revealing a linear relationship between stellar mass and mass-loss rates, and providing analytical models for use in planet formation simulations.

Contribution

It extends previous work by deriving new analytical relations for disc mass-loss rates as a function of stellar mass, focusing on stars between 0.1 and 1 solar mass.

Findings

Mass-loss rates scale linearly with stellar mass when X-ray luminosity varies accordingly.

Lower disc aspect ratios allow X-ray irradiation to reach larger radii, affecting mass-loss.

Models predict the observed trend of inner-disc lifetime decreasing with stellar mass.

Abstract

The strong X-ray irradiation from young solar-type stars may play a crucial role in the thermodynamics and chemistry of circumstellar discs, driving their evolution in the last stages of disc dispersal as well as shaping the atmospheres of newborn planets. In this paper we study the influence of stellar mass on circumstellar disc mass-loss rates due to X-ray irradiation, extending our previous study of the mass-loss rate's dependence on the X-ray luminosity and spectrum hardness. We focus on stars with masses between 0.1 and 1 Solar mass, which are the main target of current and future missions to find potentially habitable planets. We find a linear relationship between the mass-loss rates and the stellar masses when changing the X-ray luminosity accordingly with the stellar mass. This linear increase is observed also when the X-ray luminosity is kept fixed because of the lower disc aspect ratio which allows the X-ray irradiation to reach larger radii. We provide new analytical relations for the mass-loss rates and profiles of photoevaporative winds as a function of the stellar mass that can be used in disc and planet population synthesis models. Our photoevaporative models correctly predict the observed trend of inner-disc lifetime as a function of stellar mass with an increased steepness for stars smaller than 0.3 Solar mass, indicating that X-ray photoevaporation is a good candidate to explain the observed disc dispersal process.