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U Scorpii was observed in outburst for the tenth time in January 2010. We obtained optical and near-infrared spectroscopy from which we derive a helium abundance of N(He)/N(H) = 0.056±0.020 from the most reliable lines available; this is lower than most other estimates and indicates that the secondary is not helium-rich, as previous studies have suggested. Velocities are found to be up to 14,000 km s−1 in broad components and up to 1,800 km s−1 in narrow line components. The reddening of U Sco is found to be E(B-V) = 0.14 ± 0.12.
Optical and near-infrared observations of novae give us useful information for understanding the diversity of nova eruptions. Classical nova V1723 Aql was discovered by F. Kabashima and K. Nishiyama on 2010 September 11. We have conducted photometric and spectroscopic observations of V1723 Aql in both optical and near-infrared (NIR) wavelength regions since its discovery. The V-band decline time by 2 mag after the maximum, t2, was ~12 d. The apparent Fe II emission lines were also seen in the optical spectra. The Rc- and Ic-band light curves exhibited rapid declines (0.16 mag d−1 in Rc) 20 days after the visual maximum, while the NIR (J, H, and Ks) showed slow decline rates (~0.07 mag d−1). This rapid reddening suggests that dust particles formed during the very early phase of the expansion in V1723 Aql.
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