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The origin of dust in galaxies is still a mystery. The majority of therefractory elements are produced in supernova explosions but it is unclear howand where dust grains condense and grow, and how they avoid destruction in theharsh environments of star-forming galaxies. The recent detection of 0.1-0.5solar masses of dust in nearby supernova remnants suggests in situ dustformation, while other observations reveal very little dust in supernovae thefirst few years after explosion. Observations of the bright SN 2010jl have beeninterpreted as pre-existing dust, dust formation or no dust at all. Here wereport the rapid (40-240 days) formation of dust in its dense circumstellarmedium. The wavelength dependent extinction of this dust reveals the presenceof very large (> 1 micron) grains, which are resistant to destructiveprocesses. At later times (500-900 days), the near-IR thermal emission shows anaccelerated growth in dust mass, marking the transition of the supernova from acircumstellar- to an ejecta-dominated source of dust. This provides the linkbetween the early and late dust mass evolution in supernovae with densecircumstellar media.

Rapid formation of large dust grains in the luminous supernova SN 2010jl