Evans, A, Kuin, P, Page, K, Mroz, P, Darnley, M, Shore, S, Osborne, J, Walter, F, Di Mille, F, Morrell, N, Munari, U, Bohlsen, T, Gehrz, R, Starrflield, S, Henze, M, Williams, S, Schwarz, G, Udalski, A, Szymanski, M, Poleski, R, Soszynski, I, Ribeiro, V, Angeloni, R, Breeveld, A, Beardmore, A and Skowron, J (2020) The January 2016 eruption of recurrent nova LMC 1968. Monthly Notices of the Royal Astronomical Society, 491 (1). pp. 655-679. ISSN 0035-8711

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We present a comprehensive review of all observations of the eclipsing recurrent Nova LMC 1968 in the Large Magellanic Cloud which was previously observed in eruption in 1968, 1990, 2002, 2010, and most recently in 2016. We derive a probable recurrence time of 6.2 ± 1.2 years and provide the ephemerides of the eclipse. In the ultraviolet-optical-IR photometry the light curve shows high variability right from the first observation around two days after eruption. Therefore no colour changes can be substantiated. Outburst spectra from 2016 and 1990 are very similar and are dominated by H and He lines longward of 2000˚A. Interstellar reddening is found to be E(B-V) = 0.07 ± 0.01. The super soft X-ray luminosity is lower than the Eddington luminosity and the X-ray spectra suggest the mass of the WD is larger than 1.3 M�. Eclipses in the light curve suggest that the system is at high orbital inclination. On day four after the eruption a recombination wave was observed in Fe II ultraviolet absorption lines. Narrow line components are seen after day 6 and explained as being due to reionisation of ejecta from a previous eruption. The UV spectrum varies with orbital phase, in particular a component of the He II 1640 ˚A emission line, which leads us to propose that early-on the inner WD Roche lobe might be filled with a bound opaque medium prior to the re-formation of an accretion disk. Both this medium and the ejecta can cause the delay in the appearance of the soft X-ray source.

Item Type: Article
Additional Information: This is the accepted author manuscript (AAM). The final published version (version of record) is available online via Oxford University Press at https://doi.org/10.1093/mnras/stz2960 - please refer to any applicable terms of use of the publisher.
Uncontrolled Keywords: novae, cataclysmic variables, stars: individual (Nova LMC 1968), ultraviolet: stars, X-rays: binaries, binaries: eclipsing
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 04 Nov 2019 12:44
Last Modified: 21 Feb 2020 15:56
URI: https://eprints.keele.ac.uk/id/eprint/7124

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