  We present infrared multi-epoch observations of the dust forming nova V1280
Sco over $\sim$2000 days from the outburst. The temporal evolution of the
infrared spectral energy distributions at 1272, 1616 and 1947 days can be
explained by the emissions produced by amorphous carbon dust of mass
(6.6--8.7)$\times$10$^{-8}$M$_{\odot}$ with a representative grain size of
0.01$~\mu$m and astronomical silicate dust of mass
(3.4--4.3)$\times$10$^{-7}$M$_{\odot}$ with a representative grain size of
0.3--0.5$~\mu$m. Both of these dust species travel farther away from the white
dwarf without an apparent mass evolution throughout those later epochs. The
dust formation scenario around V1280 Sco suggested from our analyses is that
the amorphous carbon dust is formed in the nova ejecta followed by the
formation of silicate dust in the expanding nova ejecta or as a result of the
interaction between the nova wind and the circumstellar medium.
