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V341 Ara was recently recognised as one of the closest (d ~ 150 pc) andbrightest (V~ 10) nova-like cataclysmic variables. This unique system issurrounded by a bright emission nebula, likely to be the remnant of a recentnova eruption. Embedded within this nebula is a prominent bow-shock, where thesystem's accretion disc wind runs into its own nova shell. In order toestablish its fundamental properties, we present the first comprehensivemulti-wavelength study of the system. Long-term photometry revealsquasi-periodic, super-orbital variations with a characteristic time-scale of10-16 days and typical amplitude of ~1 mag. High-cadence photometry from TESSreveals for the first time both the orbital period and a "negative superhump"period. The latter is usually interpreted as the signature of a tiltedaccretion disc. We propose a recently developed disc instability model as aplausible explanation for the photometric behaviour. In our spectroscopic data,we clearly detect anti-phased absorption and emission line components. Theirradial velocities suggest a high mass ratio, which in turn implies an unusuallylow white dwarf mass. We also constrain the wind mass-loss rate of the systemfrom the spatially resolved [O iii] emission produced in the bow-shock; thiscan be used to test and calibrate accretion disc wind models. We suggest apossible association between V341 Ara and a "guest star" mentioned in Chinesehistorical records in AD1240. If this marks the date of the system's novaeruption, V341 Ara would be the oldest recovered nova of its class and anexcellent laboratory for testing nova theory.

Bow-shocks, nova shells, disc winds and tilted discs: The Nova-Like V341 Ara Has It All