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A long-standing question related to nova eruptions is how these eruptions canlead to the formation of dust despite the ostensibly inhospitable environmentfor dust within the hot, irradiated ejecta. Novae in systems such as thesymbiotic binary RS Oph offers a articularly clear view of some nova shocks andany associated dust production. Here we use spectropolarimetric monitoring ofthe RS Oph starting two days after its eruption in 2021 Aug. to show that: dustwas present in the RS Oph system as early as two days into the 2021 eruption;the spatial distribution of this early dust was asymmetric, with componentsboth aligned with and perpendicular to the orbital plane of the binary; betweentwo and nine days after the start of the eruption, this early dust wasgradually destroyed; and dust was again created, aligned roughly with theorbital plane of the binary, more than 80 days after the start of the outburst,most likely as a result of shocks that arose as the ejecta interacted withcircumbinary material concentrated in the orbital plane. Modelling of X-raysand very-high energy GeV and TeV emission from RS Oph days to months into the2021 eruption suggests that collisions between the ejecta and the circumbinarymaterial may have led to shock formation in two regions: the polar -perpendicular to the orbital plane where collimated outflows have been observedafter prior eruptions, and a circumbinary torus in the orbital plane. Theobservations described here indicate that dust formed in approximately the sametwo regions, supporting the connection between shocks and dust in novae andrevealing a very early onset of asymmetry. The spectropolarimetric signaturesof RS Oph in the first week into the 2021 outburst indicate: polarized fluxacross the H{\alpha} emission line and position angle orientation relative tothe radio axis are similar to the spectropolarimetric signatures of AGNs.

Transient and asymmetric dust structures in the TeV-bright nova RS Oph revealed by spectropolarimetry