Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation. Issue 3 (29th December 2021)

• Record Type: Journal Article
• Authors: Kumar, Vipin; Srivastava, Mudit K; Banerjee, Dipankar P K; Woodward, C E; Munari, Ulisse; Evans, Aneurin; Joshi, Vishal; Dallaporta, Sergio; Page, Kim L
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 510:Issue 3(2022)
• Page Start: 4265
• Page End: 4283
• Publication Date: 2021-12-29
• Subjects: line: identification -- stars: individual V2891 Cyg -- stars: novae, cataclysmic variables -- techniques: photometric, spectroscopic -- infrared: spectra; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab3772
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present multi-epoch optical and near-infrared observations of the highly reddened, Fe ii class slow Nova V2891 Cygni. The observations span 15 months since its discovery. The initial rapid brightening from quiescence, and the presence of an ∼35-d long pre-maximum halt, is well documented. The evidence that the current outburst of V2891 Cyg has undergone several distinct episodes of mass ejection is seen through time-varying P Cygni profiles of the O i 7773 Å line. A highlight is the occurrence of a dust formation event centred around approximately +273 d, which coincides with a phase of coronal line emission. The dust mass is found to be $\sim\!{0.83{-}1.25} \times 10^{-10}\ \mathrm{M}_{\odot }$ . There is strong evidence to suggest that the coronal lines are created by shock heating rather than by photoionization. The simultaneous occurrence of the dust and coronal lines (with varying velocity shifts) supports the possibility that dust formation is shock induced. Such a route for dust formation has not previously been seen in a nova, although the mechanism has been proposed for dust formation in some core-collapse supernovae. Analysis of the coronal lines indicates a gas mass and temperature of 8.35–8.42 × 10 −7 M⊙ and ∼(4.8–9.1) × 10 5 K, respectively, and an overabundance of aluminium and silicon. A Case B analysis of the hydrogen lines yields a mass of the ionized gas of (8.60 ± 1.73) × 10 −5 M⊙ . The reddening and distance to the nova are estimated to be E ( B − V ) = 2.21 ± 0.15 and d = 5.50 kpc, respectively.