Open AccessAn analysis of the spectra and light curve of Nova Centauri 1995
Author(s) -
Yan Tse James,
Hearnshaw J. B.,
Rosenzweig P.,
Guzman E.,
Escalona O.,
Gilmore A. C.,
Kilmartin P. M.,
Watson L. C.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04300.x
Subject(s) - physics , nova (rocket) , light curve , astrophysics , spectral line , emission spectrum , astronomy , amplitude , optics , aeronautics , engineering
The light curve and spectra of Nova Centauri 1995 (V888 Cen) are analysed. The spectra were obtained a few days post‐maximum. The nova is found to be a very fast nova, declining by 2 mag within about 5±2 d of maximum. The light curve shows strong oscillations in the transition region, of peak‐to‐peak amplitude about 1.5 mag and period 12–15 d. The light curve of Nova Centauri resembles closely that of Nova Aquilae 1918 (V603 Aql). The early blue and red spectra obtained at Mt John show broad emission lines, many with P Cygni profiles. The absorption lines are found in two velocity systems at about −1765 and −3010 km s −1 , in respectively the principal and diffuse‐enhanced stages of spectral development, as defined by McLaughlin. Nova Centauri has many Fe ii lines in emission, indicating that it is a member of the Williams Fe ii class of classical novae.