Speaker
Description
V2487 Oph is a recurrent nova that underwent a fast and luminous eruption in 1998 (t₃ ≈ 8 days, peak magnitude 9.5). The host system hosts a massive white dwarf (~1.35 M☉) accreting from a donor star (~0.21 M☉) in a binary with an orbital period of 0.753 days (~18.1 hours). Previous X-ray observations conducted 2.7 and 3.2 years after the outburst suggested that accretion had resumed in the system. Here, we present the X-ray analysis of five observations of V2487 Oph obtained with XMM-Newton and Suzaku over 12 years following the 1998 eruption, characterising the long-term X-ray behaviour of the system and examining evidence for sustained or re-established accretion during the post-nova phase. We also include preliminary NewAthena simulations to evaluate how future high-resolution X-ray observations could improve the detection and characterisation of nova host systems.
