Journal Article

The photometric period in ES Ceti

C. M. Copperwheat, T. R. Marsh, V. S. Dhillon, S. P. Littlefair, P. A. Woudt, B. Warner, J. Patterson, D. Steeghs, J. Kemp, E. Armstrong and R. Rea

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 413, issue 4, pages 3068-3074
Published in print June 2011 | ISSN: 0035-8711
Published online May 2011 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2011.18382.x
The photometric period in ES Ceti

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We present ULTRACAM photometry of ES Cet, an ultracompact binary with a 620-s orbital period. The mass transfer in systems such as this one is thought to be driven by gravitational radiation, which causes the binary to evolve to longer periods since the semidegenerate donor star expands in size as it loses mass. We supplement these ULTRACAM+William Herschel Telescope (WHT) data with observations made with smaller telescopes around the world over a 9-yr baseline. All of the observations show variation on the orbital period, and by timing this variation we track the period evolution of this system. We do not detect any significant departure from a linear ephemeris, implying a donor star that is of small mass and close to a fully degenerate state. This finding favours the double white dwarf formation channel for this AM Canum Venaticorum (AM CVn) star. An alternative explanation is that the system is in the relatively short-lived phase in which the mass transfer rate climbs towards its long-term value.

Keywords: binaries: close; stars: individual: ES Ceti; novae, cataclysmic variables; white dwarfs

Journal Article.  5610 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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