Inferring the Gas-to-Dust Ratio in the Main Planet-Forming Region of Disks

Abstract

Measuring the amount of gas and dust in protoplanetary disks is a key challenge in planet formation studies. Here we provide a new set of dust depletion factors and relative mass surface densities of gas and dust for the innermost regions of a sample of protoplanetary disks. We do this by combining stellar theory with observed refractory element abundances in both disk hosts and open cluster stars. Our results are independent of, and complementary to, those obtained from spatially resolved disk observations.

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References in corpus (6)

• Mass measurements in protoplanetary disks from hydrogen deuteride
• HD far infrared emission as a measure of protoplanetary disk mass
• Mass constraints for 15 protoplanetary disks from HD 1-0
• Measuring protoplanetary disk gas surface density profiles with ALMA
• C${}^{18}$O emission as an effective measure of gas masses of protoplanetary disks
• A spectroscopic study of the open cluster NGC 6250