Fig. 4: Size of the smallest granules on the surface of R Doradus determined using ALMA compared with theoretical predictions and the previous Very Large Telescope Interferometer measurement for π1 Gruis10.
From: One month convection timescale on the surface of a giant evolved star
The observations are plotted versus log[g], and the 1σ s.d. error bars include the uncertainty on the distance and stellar mass. The solid black lines indicate the parametric scaling presented in this paper. The thick line was calculated for a stellar effective temperature Teff = 2,710 K, which is the value for R Doradus. The thin line is the same model for Teff = 3,200 K, which is closer to the value for π1 Gruis. The other lines (dotted25, dashed29 and dash-dotted19) represent parametric models from the literature, with the thick and thin lines calculated for the stellar temperatures of 2,710 and 3,200 K, respectively. For the model from ref. 19, we assume solar metallicity. VLTI, Very Large Telescope Interferometer.
