Fig. 2
Midplane temperature of our disk model, which assumes that viscous heating is the dominant heating term. Examples for three different local disk opacities (κ, in m2 kg−1) are shown. The black line with κ = 10−7m2 kg−1 is our nominal disk model. With respect to the abscissa, we note that young solar-type stars can have radii of 0.01 AU (about two solar radii) or more.
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