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The origin of the very red optical and infrared colours of intermediate-age($\sim$10 - 500 Myr) L-type dwarfs remains unknown. It has been suggested thatlow-gravity atmospheres containing large amounts of dust may account for theobserved reddish nature. We explored an alternative scenario by simulatingprotoplanetary and debris discs around G196-3B, which is an L3 young browndwarf with a mass of $\sim 15$ $M_{\rm Jup}$ and an age in the interval 20 -300 Myr. The best-fit solution to G196-3B's photometric spectral energydistribution from optical wavelengths through 24 $\mu$m corresponds to thecombination of an unreddened L3 atmosphere ($T_{\rm eff} \approx 1870$~K) and awarm ($\approx$ 1280 K), narrow ($\approx$ 0.07 - 0.11 R$_{\odot}$) debris disclocated at very close distances ($\approx$ 0.12 - 0.20 R$_{\odot}$) from thecentral brown dwarf. This putative, optically thick, dusty belt, whose presenceis compatible with the relatively young system age, would have a mass $\ge7\times 10^{-10}$ M$_{\oplus}$ comprised of sub-micron/micron characteristicdusty particles with temperatures close to the sublimation threshold ofsilicates. Considering the derived global properties of the belt and thedisc-to-brown dwarf mass ratio, the dusty ring around G196-3B may resemble therings of Neptune and Jupiter, except for its high temperature and thickvertical height ($\approx 6 \times 10^3$ km). Our inferred debris disc model isable to reproduce G196-3B's spectral energy distribution to a satisfactorylevel of achievement.

Spectral energy distribution simulations of a possible ring structure around the young, red brown dwarf G196-3B