Determine the stellar-mass scaling of metal-enriched gas accretion

Determine how the accretion of heavy-element-enriched disk gas by giant planets scales with stellar mass, including the contribution of volatiles evaporated from pebbles as they cross their ice lines.

Background

The formation model developed in the paper accounts for heavy-element enrichment through solid accretion but does not include the accretion of metals dissolved in disk gas. Volatiles released from pebbles can increase the local gas metallicity, and giant planets may acquire substantial heavy-element masses through accreting this enriched gas.

Because the observed metallicity of GEMS should combine contributions from solid and gas accretion, determining the stellar-mass dependence of this channel is necessary for constructing formation models that consistently couple planetary growth with disk chemical evolution.