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We present infrared spectroscopy of the 2019 eruption of the recurrent novaV3890 Sgr, obtained over the period 5.1-46.3 days after the eruption. Thespectrum of the red giant became more prominent as the flux declined, and byday 46.3 dominated the spectrum. Hydrogen and helium emission lines consistedof a narrow component superposed on a broad pedestal. The full width at halfmaximum of the narrow components declined with time $t$ as the eruptionprogressed, as ${t}^{-0.74}$, whereas those of the broad components remainedessentially constant. Conversely, the line fluxes of the narrow components ofPa,$\beta$ remained roughly constant, while those of the broad componentsdeclined by a factor $\sim30$ over a period of $\lesssim25$~days. The behaviourof the broad components is consistent with them arising in unencumberedfast-flowing ejecta perpendicular to the binary plane, in material that wasejected in a short $\sim3.3$-day burst. The narrow components arise in materialthat encounters the accumulated circumstellar material. The outburst spectrawere rich in coronal lines. There were two coronal line phases, one thatoriginated in gas ionised by supersoft X-ray source, the other in shocked gas.From the relative fluxes of silicon and sulphur coronal lines on day 23.4 -when the emitting gas was shocked - we deduce that the temperature of thecoronal gas was $9.3\times10^5$~K, and that the abundances are approximatelysolar.

Infrared spectroscopy of the 2019 eruption of the recurrent nova V3890 Sgr: separation into equatorial and polar winds revealed