tokens: This is due not to continual acceleration, but instead to previously higher velocities and higher mass loss rates earlier in the model’s evolution. In Figure 4 , we show the linear (left-hand plot) and logarithmic (right-hand plot) temporal evolution of our main fiducial model as well as fiducial models with different WD and envelope masses. Black, red, and green lines represent core + envelope masses of , , and , respectively. In each plot, the top panel shows the evolution of the total luminosity, which is the sum of the luminosity at an optical depth of and the power from positron kinetic energy released by decays above the photosphere. We assume the positrons are able to thermalize and deposit their energy locally while the gamma-rays emitted during the and decays escape the wind and the surrounding SN ejecta. In practice, however, the positron kinetic energy in the optically thin region is smaller than the luminosity at the photosphere, so this contribution is not significant. Note that the luminosity from the SN Ia ejecta is not included. For comparison, the dotted line in the top panels represents the total power from radioactive decays of of initially pure under “lab” conditions. Figure 4. Evolution of winds launched from post-SN Ia surviving WD donors with envelope masses determined by the maximum bound ejecta mass. Three different models are shown, with core + envelope masses of (black), (red), and (green). The left-hand and right-hand plots use linear and logarithmic time axes, respectively. The top panel in each plot shows the sum of the luminosity at the photosphere and the luminosity from thermalization of positron kinetic energy from decays above the photosphere. The dotted line represents the total power from radioactive decays of of initially pure under “lab” conditions. Note that the luminosity from the SN Ia ejecta is not included. The middle panels track the effective temperature at the location. The bottom panels show the velocity at the photosphere (solid) and the mass-averaged velocity of material above the photosphere (dashed). The effective temperature, derived from the luminosity and radius at the surface, is shown in the middle panels. The velocity at the location is shown as a solid line in the bottom panels, and the mass-averaged velocity in the optically thin region is shown as a dashed line. The observed quasi-bolometric late-time light curve of the best observed SN Ia to date, SN 2011fe, is shown as bullets (Nugent et al. 2011 ; Tsvetkov et al. 2013 ; Kerzendorf et al. 2014 ; Shappee et al. 2016 ). The late-time flattening of SN 2011fe and other SNe Ia above simple predictions for decay within the SN ejecta has been attributed to light echoes and the decay of long-lived radioactive isotopes such as 57 Co and 55 Fe (Seitenzahl et al. 2009 ; Röpke et al. 2012 ; Kerzendorf et al. 2014 ; Graur et al. 2016 ; Shappee et al. 2016 ). Our models represent an additional contribution to the total luminosity, and
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