Fig. 1
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Initial conditions for density (above) and temperature (below), obtained using the iterative procedure described in Sect. 2.3. White lines indicate the corresponding cooling-time contours, computed using Eq. (8). Due to our constant dust-to-gas ratio and assumption of small dust grains throughout the disk, we obtain shorter radiative–diffusion and gas–grain coupling times than in Bae et al. (2021).
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