Total modelled dust masses versus post-explosion time for the various SN cases considered in this study and dust masses derived from mid-IR data for a sample of Type II-P SNe-SN1987A (Wooden et al. 1993; Ercolano et al. 2007), SN1999em (Elmhamdi et al. 2003), SN2003gd (Sugerman et al. 2006; Meikle et al. 2007), SN2003J (Szalai & Vinkó 2013), SN2004dj (Szalai et al. 2011; Meikle et al. 2011), SN2004et (Kotak et al. 2009), SN2004A (Szalai & Vinkó 2013), SN2005af (Kotak 2008), SN2006bp (Gallagher et al. 2012; Szalai & Vinkó 2013), SN2007it (Andrews et al. 2011), SN2007od (Inserra et al. 2011; Andrews et al. 2010). The bars associated with the data points indicate the range of mass values derived from various authors or models for a specific SN. Full blue and red lines: 19  M_⊙ and 15  M_⊙ homogeneous ejecta, respectively. Green dotted line: low ⁵⁶Ni mass, 15  M_⊙ homogeneous ejecta. Brown dotted line: 19  M_⊙ clumpy ejecta. The dust masses derived for the young remnant SN1987A and the Crab Nebula are also shown (SN1987A – Matsuura et al. 2011; Indebetouw et al. 2014, The Crab – Gomez et al. 2012; Temim & Dwek 2013).