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Title:
Binaries discovered by the SPYproject. IV. Five single-lined DA double white dwarfs
Authors:
Nelemans, G.; Napiwotzki, R.; Karl, C.; Marsh, T. R.; Voss, B.; Roelofs, G.; Izzard, R. G.; Montgomery, M.; Reerink, T.; Christlieb, N.; Reimers, D.
Affiliation:
AA(Department of Astrophysics, Radboud University Nijmegen, PO Box 9010 6500 GL, Nijmegen, The Netherlands ; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AB( Centre for Astrophysics Research, University of Hertfordshire, Hatfield, AL10 9AB, UK ), AC( Remeis-Sternwarte, Universität Erlangen-Nürnberg, Sternwartestr. 7, 96049 Bamberg, Germany ), AD( Department of Physics, University of Warwick, Coventry CV4 7AL, UK ), AE( Institut für Theoretische Physik und Astrophysik, University of Kiel, 24098 Kiel, Germany ), AF( Department of Astrophysics, Radboud University Nijmegen, PO Box 9010 6500 GL, Nijmegen, The Netherlands), AG( Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK The Carolune Institute for Quality Astronomy, www.ciqua.org, UK ), AH( Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK ), AI( Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands ), AJ( Hamburger Sternwarte, Universität Hamburg, Gojensbergweg 112, 21029 Hamburg, Germany ), AK( Hamburger Sternwarte, Universität Hamburg, Gojensbergweg 112, 21029 Hamburg, Germany )
Publication:
Astronomy and Astrophysics, Volume 440, Issue 3, 2005, pp.1087-1095 (A&A Homepage)
Publication Date:
09/2005
Origin:
EDP Sciences
Keywords:
stars: binaries: close, stars: supernovae: general, stars: white dwarfs
DOI:
10.1051/0004-6361:20053174
Bibliographic Code:
2005A&A...440.1087N

Abstract

We present results from our ongoing follow-up observations of double

white dwarf binaries detected in the ESOÂSNÂIaÂProgenitor 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.


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