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| dc.contributor.author | Raj, A | |
| dc.contributor.author | Das, R. K | |
| dc.contributor.author | Walter, F. M | |
| dc.date.accessioned | 2020-11-17T14:22:10Z | |
| dc.date.available | 2020-11-17T14:22:10Z | |
| dc.date.issued | 2017-02-01 | |
| dc.identifier.citation | The Astrophysical Journal, Vol. 835, No. 2, 274 | en_US |
| dc.identifier.issn | 0004-637X | |
| dc.identifier.uri | http://prints.iiap.res.in/handle/2248/7148 | |
| dc.description | Restricted Access © The American Astronomical Society https://doi.org/10.3847/1538-4357/835/2/274 | en_US |
| dc.description.abstract | We present optical spectrophotometric and near-infrared (NIR) photometric observations of the nova V2676 Oph covering the period from 2012 March 29 through 2015 May 8. The optical spectra and photometry of the nova have been taken from SMARTS and Asiago; the NIR photometry was obtained from SMARTS and Mt. Abu. The spectra were dominated by strong H i lines from the Balmer series, Fe ii, N i, and [O i] lines in the initial days, typical of an Fe ii type nova. The measured FWHM for the Hβ and Hα lines was 800–1200 km s−1. There was pronounced dust formation starting 90 days after the outburst. The J − K color was the largest among recent dust-forming novae. | en_US |
| dc.language.iso | en | en_US |
| dc.publisher | IOP Publishing | en_US |
| dc.subject | Infrared: stars | en_US |
| dc.subject | Line: identification | en_US |
| dc.subject | Novae, cataclysmic variables|| | en_US |
| dc.subject | Stars: individual ( V2676 Oph )|| | en_US |
| dc.subject | Techniques: spectroscopic | en_US |
| dc.title | Optical and Near-infrared Study of Nova V2676 Oph 2012 | en_US |
| dc.type | Article | en_US |
