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Fig. 7. (Left panel) millimeter-centimeter wave spectral energy distribution of the UX Ori and CQ Tau systems; (right panel) disk model families for the millimeter integrated flux and spectral index, for a given value of the dust opacity index ยก3 and disk radius, disk model predictions move along the lines depending on the total disk mass, the higher the mass the higher the mm flux until the disk becomes optically thick and the flux saturates. Low resolution observations that do not constrain the disk size are consistent with either large, mostly optically thin disks with low values of 3 or small, optically thick disks with any value of 3- Adapted from [30]

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