Abstract
We present a detailed study of the 2016 eruption of nova V407 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 days 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 ($t_2 \leq$ 2.9 d), suggesting that the white dwarf is likely massive ($\gtrsim 1.25$ M$_{\odot}$). 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.
Highlights
Classical novae (CNe) are stellar eruptions that take place within the surface layers of accreting white dwarfs (WDs) in cataclysmic variable (CV) systems
We present a detailed study of the 2016 eruption of nova V407 Lupi (ASASSN-16kt), including optical, near-infrared, X-ray, and ultraviolet data from Southern African Large Telescope (SALT), Small and Moderate Aperture Research Telescope System (SMARTS), Southern Astrophysical Research (SOAR), Chandra, Swift, and XMM-Newton
In this paper we present a multiwavelength study of nova V407 Lupi which was discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN)1 on HJD 2457655.5 (2016 September 24.0 UT; Stanek et al 2016) at V = 9.1 and is located at equatorial coordinates of (α, δ)J2000.0 = (15h29m01.82s, –44◦49 40 .89) and Galactic coordinates of (l, b) = (330◦.09, 9◦.573)
Summary
Classical novae (CNe) are stellar eruptions that take place within the surface layers of accreting white dwarfs (WDs) in cataclysmic variable (CV) systems. These are interacting binaries consisting of a WD primary accreting from a secondary that typically fills its Roche lobe (see, e.g., Warner 1995). The fast expanding envelope moves together with the optical photosphere (Hachisu & Kato 2006, 2014), in what is known as the “fireball stage” During this the brightness of the star increases by 8 up to 15 mag (Payne-Gaposchkin 1964) and reaches its maximum visual brightness when the optical photosphere attains its maximum radius (Warner 1995; Hachisu & Kato 2014). Following the TNR, the remaining hydrogen-rich, accreted envelope continuously burns on the WD surface and may become visible when the expanding ejecta become optically thin
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