EDP Sciences
Free access
Issue A&A
Volume 440, Number 3, September IV 2005
Page(s) 1087 - 1095
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20053174



A&A 440, 1087-1095 (2005)
DOI: 10.1051/0004-6361:20053174

Binaries discovered by the SPY project

IV. Five single-lined DA double white dwarfs
G. Nelemans1, 2, R. Napiwotzki3, C. Karl4, T. R. Marsh5, B. Voss6, G. Roelofs1, R. G. Izzard2, 7, M. Montgomery2, T. Reerink8, N. Christlieb9 and D. Reimers9

1  Department of Astrophysics, Radboud University Nijmegen, PO Box 9010 6500 GL, Nijmegen, The Netherlands
    e-mail: nelemans@astro.ru.nl
2  Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
3  Centre for Astrophysics Research, University of Hertfordshire, Hatfield, AL10 9AB, UK
4  Remeis-Sternwarte, Universität Erlangen-Nürnberg, Sternwartestr. 7, 96049 Bamberg, Germany
5  Department of Physics, University of Warwick, Coventry CV4 7AL, UK
6  Institut für Theoretische Physik und Astrophysik, University of Kiel, 24098 Kiel, Germany
7  The Carolune Institute for Quality Astronomy, www.ciqua.org, UK
8  Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
9  Hamburger Sternwarte, Universität Hamburg, Gojensbergweg 112, 21029 Hamburg, Germany

(Received 1 April 2005 / Accepted 6 June 2005)

Abstract
We present results from our ongoing follow-up observations of double white dwarf binaries detected in the ESO SN Ia Progenitor SurveY (SPY). We discuss our observing strategy and data analysis and present the orbital solutions of five close double white dwarf binaries: HE0320-1917, HE1511-0448, WD0326-273, WD1013-010 and WD1210+140. Their periods range from 0.44 to 3.22 days. In none of these systems we find any spectral lines originating from the companion. This rules out main sequence companions and indicates that the companion white dwarfs are significantly older and cooler than the bright component. Infrared photometry suggests the presence of a cool, helium-rich white dwarf companion in the binary WD 0326-273. We briefly discuss the consequences of our findings for our understanding of the formation and evolution of double white dwarfs.


Key words: stars: binaries: close -- stars: supernovae: general -- stars: white dwarfs

SIMBAD Objects



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Editor-in-Chief: T. Forveille
Letters Editor-in-Chief: J. Alves
Managing Editor: C. Bertout

ISSN: 0004-6361 ; e-ISSN: 1432-0746
Frequency: 12 volumes per year
Published by: EDP Sciences

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