Time-dependent response of protoplanetary disk temperature to an FU Ori-type luminosity outburst

Open Access

Fig. 2.

Left panel: Spectral energy distributions for different stages of the outburst. The profiles for Model P and Model A are shown with dashed and solid lines, respectively. Right panel: Evolution of the corresponding radiation fluxes for several wavelengths. The reference ratio $(L_{⋆} + L_{acc}^{UV}) / L_{⋆}$ $(L_\star + L_{\mathrm{acc}}^{\mathrm{UV}})/L_\star$ for Model P is shown with a dotted line.

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