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One of the great challenges in understanding stars is measuring their masses.The best methods for measuring stellar masses include binary interaction,asteroseismology and stellar evolution models, but these methods are not idealfor red giant and supergiant stars. In this work, we propose a novel method forinferring stellar masses of evolved red giant and supergiant stars usinginterferometric and spectrophotometric observations combined with sphericalmodel stellar atmospheres to measure what we call the stellar mass index,defined as the ratio between the stellar radius and mass. The method is basedon the correlation between different measurements of angular diameter, used asa proxy for atmospheric extension, and fundamental stellar parameters. For agiven star, spectrophotometry measures the Rosseland angular diameter whileinterferometric observations generally probe a larger limb-darkened angulardiameter. The ratio of these two angular diameters is proportional to therelative extension of the stellar atmosphere, which is strongly correlated tothe star's effective temperature, radius and mass. We show that thesecorrelations are strong and can lead to precise measurements of stellar masses.

Stellar atmospheres, atmospheric extension and fundamental parameters: weighing stars using the stellar mass index