THE DUSTY NOVA V1065 CENTAURI (NOVA CEN 2007): A SPECTROSCOPIC ANALYSIS OF ABUNDANCES AND DUST PROPERTIES
- Department of Astronomy, School of Physics and Astronomy, 116 Church Street S.E., University of Minnesota, Minneapolis, MN 55455 (United States)
- Department of Physics and Astronomy, Z 3800, Stony Brook University, Stony Brook, NY, 11794-3800 (United States)
- Department of Geology and Astronomy, West Chester University, 750 South Church Street, West Chester, PA 19383 (United States)
- American Astronomical Society, 2000 Florida Avenue, NW, Suite 400, Washington, DC 20009 (United States)
- Astrophysics Group, Keele University, Keele, Staffordshire ST5 5BG (United Kingdom)
- XMM-Newton Observatory SOC, European Space Astronomy Centre, Apartado 78, 28691 Villanueva de la Canada, Madrid (Spain)
- Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)
- NASA Goddard Space Flight Center, Code 665, Greenbelt, MD 20771 (United States)
- Landessternwarte-Zentrum fuer Astronomie der Universitaet, Koenigstuhl, D-69117 Heidelberg (Germany)
- Institute for Nova Studies, Casilla 5022, Vina del Mar (Chile)
- Aerospace Corporation, Mail Stop 2-266, P.O. Box 92957, Los Angeles, CA 90009-2957 (United States)
- Dipartimento di Fisica 'Enrico Fermi', Universita di Pisa, largo Pontecorvo 3, Pisa 56127 (Italy)
- School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287 (United States)
- Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)
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{sup +2.8}{sub -2.1} kpc. The optical spectral evolution is classified as P {sup o}{sub fe} N{sub ne} A{sub o} 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 M{sub g} = (1.6 {+-} 0.2) x 10{sup -4} M{sub sun}. 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, M{sub d} , of order (0.2-3.7) x 10{sup -7} M{sub sun}, 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.
- OSTI ID:
- 21443189
- Journal Information:
- Astronomical Journal (New York, N.Y. Online), Vol. 140, Issue 5; Other Information: DOI: 10.1088/0004-6256/140/5/1347; ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
COSMOLOGY AND ASTRONOMY
ABUNDANCE
CLASSIFICATION
COLOR
DUSTS
ENERGY SPECTRA
MASS
NEON
NOVAE
PHOTOIONIZATION
SILICATES
SIMULATION
SPECTROMETERS
SPECTROPHOTOMETRY
STAR EVOLUTION
BINARY STARS
ELEMENTS
ERUPTIVE VARIABLE STARS
EVOLUTION
FLUIDS
GASES
IONIZATION
MEASURING INSTRUMENTS
NONMETALS
OPTICAL PROPERTIES
ORGANOLEPTIC PROPERTIES
OXYGEN COMPOUNDS
PHYSICAL PROPERTIES
RARE GASES
SILICON COMPOUNDS
SPECTRA
STARS
VARIABLE STARS