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An evolved donor star in the long-period cataclysmic variable HS 0218+3229

Rodríguez-Gil, P. and Torres, M. A. P. and Gänsicke, B. T. and Muñoz-Darias, T. and Steeghs, D. and Schwarz, R. and Rau, A. and Hagen, H.-J. (2009) An evolved donor star in the long-period cataclysmic variable HS 0218+3229. Astronomy and Astrophysics, 496 (3). pp. 805-812. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20090918-134803606

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Abstract

Context. We present time-resolved spectroscopy and photometry of HS 0218+3229, a new long-period cataclysmic variable discovered within the Hamburg Quasar Survey. It is one of the few systems that allow a dynamical measurement of the masses of the stellar components. Aims. We combine the analysis of time-resolved optical spectroscopy and R-band photometry with the aim of measuring the mass of the white dwarf and the donor star and the orbital inclination. Methods. Cross-correlation of the spectra with K-type dwarf templates is used to derive the radial velocity curve of the donor star. An optimal subtraction of the broadened templates is performed to measure the rotational broadening and constrain the spectral type of the donor. Finally, an ellipsoidal model is fitted to the R-band light curve to obtain constraints upon the orbital inclination of the binary system. Results. The orbital period of HS 0218+3229 is found to be 0.297229661 ± 0.000000001 d (7.13351186 ± 0.00000002 h), and the amplitude of the donor’s radial velocity curve is K_2 = 162.4 ± 1.4 km s^(−1). Modelling the ellipsoidal light curves gives an orbital inclination in the range i = 59◦ ±3◦. A rotational broadening between 82.4±1.2 km s^(−1) and 89.4±1.3 km s^(−1) is found when assuming zero and continuum limb darkening, respectively. The secondary star has most likely a spectral type K5 and contributes ∼80–85% to the R-band light. Our analysis yields a mass ratio of 0.52 < q < 0.65, a white dwarf mass of 0.44 < M_1(M_⊙) < 0.65, and a donor star mass of 0.23 < M_2(M_⊙) < 0.44. Conclusions. We find that the donor star in HS 0218+3229 is significantly undermassive for its spectral type. It is therefore very likely that it has undergone nuclear evolution prior to the onset of mass transfer.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/200811312DOIArticle
ORCID:
AuthorORCID
Gänsicke, B. T.0000-0002-2761-3005
Rau, A.0000-0001-5990-6243
Additional Information:© ESO 2009. Received 7 November 2008. Accepted 20 January 2009. This work was supported by XMM-Newton Grant NNG05GJ22G. The HQS was supported by the Deutsche Forschungsgemeinschaft through grants Re 353/11 and Re 353/22. The use of the MOLLY package developed and maintained by Tom Marsh is acknowledged. Thanks to the anonymous referee for valuable input.
Funders:
Funding AgencyGrant Number
NASANNG05GJ22G
Deutsche Forschungsgemeinschaft (DFG)353/11
Deutsche Forschungsgemeinschaft (DFG)353/22
Subject Keywords:accretion, accretion discs; stars: binaries: close; stars: novae, cataclysmic variables
Issue or Number:3
Record Number:CaltechAUTHORS:20090918-134803606
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20090918-134803606
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:15983
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:22 Sep 2009 22:30
Last Modified:22 Nov 2019 05:33

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