A disc evolution model with a 40 au centrifugal radius and weak viscous heating best reproduces the flux-size relation of young protoplanetary discs, while older discs are mostly optically thin at 1.3 mm.
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The evolution of the flux-size relationship in protoplanetary discs by viscous evolution and radial pebble drift
A disc evolution model with a 40 au centrifugal radius and weak viscous heating best reproduces the flux-size relation of young protoplanetary discs, while older discs are mostly optically thin at 1.3 mm.