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We present multi-epoch optical and near-infrared observations of the highlyreddened, \pion{Fe}{ii} class slow nova V2891 Cygni. The observations span 15months since its discovery. The initial rapid brightening from quiescence, andthe presence of a $\sim$35 day long pre-maximum halt, is well documented. Theevidence that the current outburst of V2891 Cyg has undergone several distinctepisodes of mass ejection is seen through time-varying P Cygni profiles of theO\,{\sc i} 7773\,$\AA$ line. A highlight is the occurrence of a dust formationevent centred around $\sim$+273d, which coincides with a phase of coronal lineemission. The dust mass is found to be $\sim0.83-1.25 \times 10^{-10}M_{\odot}$. There is strong evidence to suggest that the coronal lines arecreated by shock heating rather than by photoionization. The simultaneousoccurrence of the dust and coronal lines (with varying velocity shifts)supports the possibility that dust formation is shock-induced. Such a route fordust formation has not previously been seen in a nova, although the mechanismhas been proposed for dust formation in some core-collapse supernovae. Analysisof the coronal lines indicates a gas mass and temperature of8.35--8.42$\times10^{-7}$ M$_\odot$ and $\sim(4.8-9.1)\times10^{5}$~Krespectively, and an overabundance of aluminium and silicon. A Case B analysisof the hydrogen lines yields a mass of the ionized gas of($8.60\pm1.73)\times10^{-5}$ M$_{\odot}$. The reddening and distance to thenova are estimated to be $E(B-V)$ = 2.21$\pm$0.15 and $d$ = 5.50 kpcrespectively.

Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation