Castro Segura, NKnigge, CAcosta-Pulido, J AAltamirano, Ddel Palacio, SHernandez Santisteban, J VPahari, MRodriguez-Gil, PBelardi, CBuckley, D A HPonomareva, Anastasia2024-03-132024-03-130035-8711http://hdl.handle.net/1885/315967V341 Ara was recently recognized as one of the closest (d~ 150 pc) and brightest (V~10) nova-like cataclysmic variables. This unique system is surrounded by a bright emission nebula, likely to be the remnant of a recent nova eruption. Embedded within this nebula is a prominent bow shock, where the system's accretion disc wind runs into its own nova shell. In order to establish its fundamental properties, we present the first comprehensive multiwavelength study of the system. Long-term photometry reveals quasi-periodic, super-orbital variations with a characteristic time-scale of 10-16 d and typical amplitude of ~1 mag. High-cadence photometry from theTransiting Exoplanet Survey Satellite (TESS) reveals for the first time both the orbital period and a 'negative superhump' period. The latter is usually interpreted as the signature of a tilted accretion disc. We propose a recently developed disc instability model as a plausible explanation for the photometric behaviour. In our spectroscopic data, we clearly detect antiphased absorption and emission-line components. Their radial velocities suggest a high mass ratio, which in turn implies an unusually low white-dwarf mass. We also constrain the wind mass-loss rate of the system from the spatially resolved [O iii] emission produced in the bow shock; this can be used to test and calibrate accretion disc wind models. We suggest a possible association between V341 Ara and a 'guest star' mentioned in Chinese historical records in AD 1240. If this marks the date of the system's nova eruption, V341 Ara would be the oldest recovered nova of its class and an excellent laboratory for testing nova theory.NCS and CK acknowledge support by the Science and Technology Facilities Council (STFC), and from STFC grant ST/M001326/1. DMH acknowledges financial assistance from the South African National Research Foundation (NRF) and the South African Astronomical Observatory. NPMK’s work was supported by the UK Space Agency. AAP acknowledges support from the STFC consolidated grant ST/S000488/1 and from the Australian Research Council grant DP150104129. DA acknowledges support from the Royal Society. JVHS acknowledges support from a STFC grant ST/R000824/1. DRAW was supported by the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. DJJ acknowledges support from the National Science Foundation award AST-1440254. DAHB acknowledges research support from the South African National Research Foundationapplication/pdfen-AU© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Societyaccretion, accretion discsbinaries: spectroscopicnovae, cataclysmic variableswinds, outflowsshock waves202110.1093/mnras/staa25162022-11-13