We present a detailed study of the 2016 eruption of novaV407 Lupi (ASASSN-16kt), including optical, near-infrared, X-ray, and ultraviolet data from SALT, SMARTS, SOAR, Chandra, Swift, and XMM-Newton. Timing analysis of the multiwavelength light curves shows that, from 168 d post-eruption and for the duration of the X-ray supersoft source phase, two periods at 565 s and 3.57 h are detected. We suggest that these are the rotational period of the white dwarf and the orbital period of the binary, respectively, and that the system is likely to be an intermediate polar. The optical light-curve decline was very fast (t2 ≤ 2.9 d), suggesting that the white dwarf is likely massive (≳ 1.25M⊙). The optical spectra obtained during the X-ray supersoft source phase exhibit narrow, complex, and moving emission lines of He II, also characteristics of magnetic cataclysmic variables. The optical and X-ray data show evidence for accretion resumption while the X-ray supersoft source is still on, possibly extending its duration.
|Original language||English (US)|
|Number of pages||38|
|Journal||Monthly Notices of the Royal Astronomical Society|
|State||Published - Oct 11 2018|
Bibliographical noteFunding Information:
A part of this work is based on observations made with the Southern African Large Telescope (SALT), under the Large Science Programme on transient 2016-2-LSP-001. EA, DB, PAW, SM, and BM gratefully acknowledge the receipt of research grants from the National Research Foundation (NRF) of South Africa. AD was supported by the Slovak grant Vega 1/0335/16 AK acknowledges the National Research Foundation of South Africa and the Russian Science Foundation (project no.14-50-00043). MO had support from a NASA-Smithsonian grant for Director Discretionary Time Chandra observations APB, KLP, NPMK, and JPO acknowledge support from the UK Space Agency. JS acknowledges support from the Packard Foundation. This paper is partially based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, Inovaçãos e Comunicaçãoes (MCTIC) do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). MJD acknowledges the partial support from the UK Science & Technology Facilities Council (STFC). SS gratefully acknowledges partial support from NASA grants to ASU. We thank B. Warner and R. E. Williams, and L. Izzo for private discussion. We acknowledge the use of observations from the AAVSO International Database and we thank the observers who obtained these observations. We thank an anonymous referee for useful comments.
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
- Cataclysmic variables
- Stars: individual (V407 Lup)
- White dwarfs