SIMBAD references

2010AJ....140.1347H - Astron. J., 140, 1347-1369 (2010/November-0)

The dusty nova V1065 Centauri (Nova Cen 2007): a spectroscopic analysis of abundances and dust properties.

HELTON L.A., WOODWARD C.E., WALTER F.M., VANLANDINGHAM K., SCHWARZ G.J., EVANS A., NESS J.-U., GEBALLE T.R., GEHRZ R.D., GREENHOUSE M., KRAUTTER J., LILLER W., LYNCH D.K., RUDY R.J., SHORE S.N., STARRFIELD S. and TRURAN J.

Abstract (from CDS):

We examine the ejecta evolution of the classical nova V1065 Centauri, constructing a detailed picture of the system based on spectrophotometric observations obtained from 9 to approximately 900 days post-outburst with extensive coverage from optical to mid-infrared wavelengths. We estimate a reddening toward the system of E(B-V) = 0.5±0.1, based upon the B - V color and analysis of the Balmer decrement, and derive a distance estimate of 8.7+2.8–2.1kpc. The optical spectral evolution is classified as P ^ o ^feNneAo according to the CTIO Nova Classification system of Williams et al. Photoionization modeling yields absolute abundance values by number, relative to solar of He/H = 1.6±0.3, N/H = 144±34, O/H = 58 ±18, and Ne/H = 316±58 for the ejecta. We derive an ejected gas mass of Mg= (1.6±0.2)x10–4 M. The infrared excess at late epochs in the evolution of the nova arises from dust condensed in the ejecta composed primarily of silicate grains. We estimate a total dust mass, Md, of order (0.2-3.7)x10–7 M, inferred from modeling the spectral energy distribution observed with the Spitzer IRS and Gemini-South GNIRS spectrometers. Based on the speed class, neon abundance, and the predominance of silicate dust, we classify V1065 Cen as an ONe-type classical nova.

Abstract Copyright:

Journal keyword(s): circumstellar matter - novae, cataclysmic variables - stars: individual (V1065 Cen, Nova Cen 2007)

Simbad objects: 21

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2010AJ....140.1347H and select 'bookmark this link' or equivalent in the popup menu


2021.03.02-00:50:16

© Université de Strasbourg/CNRS

    • Contact