TY - JOUR
T1 - Multiwavelength observations of V407 Lupi (ASASSN-16kt) - a very fast nova erupting in an intermediate polar
AU - Aydi, E.
AU - Orio, M.
AU - Beardmore, A. P.
AU - Ness, J. U.
AU - Page, K. L.
AU - Kuin, N. P.M.
AU - Walter, F. M.
AU - Buckley, D. A.H.
AU - Mohamed, S.
AU - Whitelock, P.
AU - Osborne, J. P.
AU - Strader, J.
AU - Chomiuk, L.
AU - Darnley, M. J.
AU - Dobrotka, A.
AU - Kniazev, A.
AU - Miszalski, B.
AU - Myers, G.
AU - Ospina, N.
AU - Henze, M.
AU - Starrfield, S.
AU - Woodward, C. E.
N1 - Publisher Copyright:
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2018/10/11
Y1 - 2018/10/11
N2 - 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.
AB - 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.
KW - Cataclysmic variables
KW - Novae
KW - Stars: individual (V407 Lup)
KW - White dwarfs
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U2 - 10.1093/mnras/sty1759
DO - 10.1093/mnras/sty1759
M3 - Article
AN - SCOPUS:85052602757
SN - 0035-8711
VL - 480
SP - 572
EP - 609
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -