Post-maximum spectroscopy of the classical nova V1112 Per (Nova Per 2020)

ATel #14243; Drahomir Chochol, Lubomir Hambalek, Richard Komzik, Theodor Pribulla, Augustin Skopal (Astronomical Institute, Slovak Academy of Sciences, Tatranska Lomnica)
on 4 Dec 2020; 16:03 UT
Credential Certification: Augustin Skopal (skopal@ta3.sk)

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The Nova Persei 2020 = V1112 Per = TCP J04291888+4354233 was discovered by Seiji Ueda on 2020 Nov 25.813 UT and classified as a classical nova by Munari et al. (ATel #14224). Pre-maximum spectroscopy obtained by Munari et al. (ATel #14229) on Nov 26.813 and 27.004 UT shows P-Cyg features for HI, OI, HeI and NII lines. In the spectra from Nov 27.703 and 27.715 all HeI and NII lines have disappeared and were replaced by FeII lines with pronounced P-Cyg absorption with respect to the emission component at -750 km/s. The HI and OI lines exhibited P-Cyg absorption at -640 km/s. The transition of the spectral characteristics from the He/N class to a Fe II class was confirmed by Borthakur et al. (ATel #14230). According to the AAVSO light curve, the nova reached the maximum in V=8.24 mag and R=7.51 mag during the flare on Nov. 29.896. Two echelle spectra (420-720 nm, resolving power 38,000) have been obtained with the 1.3-m telescope + MUSICOS-design spectrograph at Skalnaté Pleso Observatory on Dec. 01.87 and 02.78 UT. Besides the Fe II lines with P-Cyg absorption at -750 km/s, the spectra are dominated by Halpha and Hbeta emission lines with FWHM 984 km/s and 947 km/s, respectively. Their P-Cyg type profiles exhibit two absorption components. The radial velocity of the slow and fast component with respect to the peak of the main emission core is -568 km/s and -1206 km/s for Halpha and -619 km/s and -1130 km/s for Hbeta line, respectively. The fast outflow is also detected as an emission bump with the radial velocity of 987 km/s and 919 km/s for Halpha and Hbeta line, respectively. While the slow component reflects the initial ejection of the accreted material, the fast component is associated with a radiation-driven wind from the white dwarf. According to Aidy et al. (arXiv:2010.07481) the secondary fast outflow is physically distinct from the first slow outflow, being originating from inside it. Chochol et al. (arXiv:2007.13337) explained the fast component in classical nova V392 Per by the approaching and receding polar outflows from the white dwarf in outburst. The Halpha profiles from our spectra are available at http://www.ta3.sk/~lhambalek/v1112per/CompareSPHa.png