Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation

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dc.contributor.author Kumar, Vipin
dc.contributor.author Srivastava, Mudit K.
dc.contributor.author Banerjee, Dipankar P. K.
dc.contributor.author Woodward, C. E.
dc.contributor.author Munari, Ulisse
dc.contributor.author Evans, Aneurin
dc.contributor.author Joshi, Vishal
dc.contributor.author Dallaporta, Sergio
dc.contributor.author Page, Kim L.
dc.coverage.spatial United Kingdom
dc.date.accessioned 2012-09-20T03:32:50Z
dc.date.available 2012-09-20T03:32:50Z
dc.date.issued 2022-03
dc.identifier.citation Kumar, Vipin; Srivastava, Mudit K.; Banerjee, Dipankar P. K.; Woodward, C. E.; Munari, Ulisse; Evans, Aneurin; Joshi, Vishal; Dallaporta, Sergio and Page, Kim L., "Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation", Monthly Notices of the Royal Astronomical Society, DOI: 10.1093/mnras/stab3772, vol. 510, no. 3, pp. 4265-4283, Mar. 2022. en_US
dc.identifier.issn 0035-8711
dc.identifier.issn 1365-2966
dc.identifier.uri http://dx.doi.org/10.1093/mnras/stab3772
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/7581
dc.description.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 ∼0.83-1.25×10-10 M⊙⁠. 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) × 105 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.
dc.description.statementofresponsibility by Vipin Kumar, Mudit K. Srivastava, Dipankar P. K. Banerjee, C. E. Woodward, Ulisse Munari, Aneurin Evans, Vishal Joshi, Sergio Dallaporta and Kim L. Page
dc.format.extent vol. 510, no. 3, pp. 4265-4283
dc.language.iso en_US en_US
dc.publisher Royal Astronomical Society en_US
dc.subject Line en_US
dc.subject Identification en_US
dc.subject Stars: individual V2891 Cyg en_US
dc.subject Stars: novae en_US
dc.subject Cataclysmic variables en_US
dc.subject Techniques: photometric en_US
dc.subject Spectroscopic en_US
dc.subject Infrared: spectra en_US
dc.title Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation en_US
dc.type Article en_US
dc.relation.journal Monthly Notices of the Royal Astronomical Society

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