EDP Sciences Journals List
Advanced Search
Subscriber Authentication Point
Home All issues Volume 386/3 Article
Free access article

Issue A&A
Volume 386, Number 3, May II 2002
Page(s) 957 - 963
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20020361



A&A 386, 957-963 (2002)
DOI: 10.1051/0004-6361:20020361

Binaries discovered by the SPY project

II. HE 1414-0848: A double degenerate with a mass close to the Chandrasekhar limit
R. Napiwotzki1, D. Koester2, G. Nelemans3, L. Yungelson4, N. Christlieb5, A. Renzini6, D. Reimers5, H. Drechsel1 and B. Leibundgut6

1  Dr. Remeis-Sternwarte, Astronomisches Institut der Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany
2  Institut für Theoretische Physik und Astrophysik, Universität Kiel, 24098 Kiel, Germany
3  Institute of Astronomy, Madingley Road, CB3 0HA Cambridge, UK
4  Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Str., 109017 Moscow, Russia
5  Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
6  European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany

(Received 19 November 2001 / Accepted 4 March 2002)

Abstract
In the course of our search for double degenerate (DD) binaries as potential progenitors of type Ia supernovae with the UVES spectrograph at the ESO VLT (ESO SN Ia Progenitor surveY - SPY) we discovered that the white dwarf HE 1414-0848 is a double-lined DA+DA binary with an orbital period of $P = 12^{{\rm h}} 25^{{\rm m}} 39^{{\rm s}}$. Semi-amplitudes of 128 km s -1 and 100 km s -1 are derived for the individual components. The amplitude ratio and the measured difference in gravitational redshift is used to estimate the masses of the individual components: $0.55~M_\odot$ and $0.71~M_\odot$. Hence the total mass of the HE 1414-0848 system is $1.26~M_\odot$, only 10% below the Chandrasekhar limit. The results of a model atmosphere analysis are consistent with our mass estimated from the orbit. Temperatures of the individual components are also determined. Possible scenarios for the formation of this system are discussed. The system will merge due to loss of angular momentum via gravitational wave radiation after two Hubble times. HE 1414-0848 does not qualify as an SN Ia progenitor, but it is the most massive close DD known today.


Key words: stars: early-type -- binaries: spectroscopic -- stars: fundamental parameters -- white dwarfs

Offprint request: R. Napiwotzki, napiwotzki@sternwarte.uni-erlangen.de

SIMBAD Objects



© ESO 2002


What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access. An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.
  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account. In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.