dc.contributor.author |
Raj, A |
|
dc.contributor.author |
Pavana, M |
|
dc.contributor.author |
Kamath, U. S |
|
dc.contributor.author |
Anupama, G. C |
|
dc.contributor.author |
Walter, F. M |
|
dc.date.accessioned |
2020-11-11T01:35:51Z |
|
dc.date.available |
2020-11-11T01:35:51Z |
|
dc.date.issued |
2018-03 |
|
dc.identifier.citation |
Acta Astronomica, Vol. 68, No. 1, pp. 79-88 |
en_US |
dc.identifier.issn |
0001-5237 |
|
dc.identifier.uri |
http://prints.iiap.res.in/handle/2248/6870 |
|
dc.description |
Restricted Access © Copernicus Foundation for Polish Astronomy; http://acta.astrouw.edu.pl/Vol68/n1/pdf/pap_68_1_4.pdf |
en_US |
dc.description.abstract |
Using our previously reported observations, we derive some physical parameters of the moderately fast nova V2676 Oph 2012 #1. The best-fit CLOUDY model of the nebular spectrum obtained
on 2015 May 8 shows a hot white dwarf source with TBB ≈ 1.0 × 105 K having a luminosity of
1.0×1038 erg/s. Our abundance analysis shows that the ejecta are significantly enhanced relative to
solar, He/H = 2.14, O/H = 2.37, S/H = 6.62 and Ar/H = 3.25. The ejecta mass is estimated to be
1.42 ×10−5 M⊙ . The nova showed a pronounced dust formation phase after 90 d from discovery.
The J −H and H −K colors were very large as compared to other molecule- and dust-forming novae in recent years. The dust temperature and mass at two epochs have been estimated from spectral
energy distribution fits to infrared photometry |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Copernicus Foundation for Polish Astronomy |
en_US |
dc.subject |
Line: identification |
en_US |
dc.subject |
Techniques: spectroscopic |
en_US |
dc.subject |
Novae, cataclysmic variables |
en_US |
dc.subject |
Stars: individual: V2676 Oph |
en_US |
dc.title |
V2676 Oph: Estimating Physical Parameters of a Moderately Fast Nova |
en_US |
dc.type |
Article |
en_US |