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Protoplanetary discs around brown dwarfs and very low mass stars offer someof the best prospects for forming Earth-sized planets in their habitable zones.To this end, we study the nature of the disc around the very low mass star V410X-ray 1, whose SED is indicative of an optically thick and very truncated dustdisc, with our modelling suggesting an outer radius of only 0.6 au. Weinvestigate two scenarios that could lead to such a truncation, and find thatthe observed SED is compatible with both. The first scenario involves thetruncation of both the dust and gas in the disc, perhaps due to a previousdynamical interaction or the presence of an undetected companion. The secondscenario involves the fact that a radial location of 0.6 au is close to theexpected location of the H$_2$O snowline in the disc. As such, a combination ofefficient dust growth, radial migration, and subsequent fragmentation withinthe snowline leads to an optically thick inner dust disc and larger, opticallythin outer dust disc. We find that a firm measurement of the CO $J=2$--1 lineflux would enable us to distinguish between these two scenarios, by enabling ameasurement of the radial extent of gas in the disc. Many models we considercontain at least several Earth-masses of dust interior to 0.6 au, suggestingthat V410 X-ray 1 could be a precursor to a system with tightly-packed innerplanets, such as TRAPPIST-1.

The extremely truncated circumstellar disc of V410 X-ray 1: a precursor to TRAPPIST-1?