Orbital period increase in ES Ceti

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Publication date

2018-01

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Ciencias Integradas

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Center

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https://hdl.handle.net/10272/23097

DOI

10.3847/1538-4357/aa9ed6

Abstract

We report a long-term study of the eclipse times in the 10 minute helium binary ES Ceti. The binary period icreases rapidly, with with P/P = 6.2 x 106 years. This is consistent with the assumption that gravitational radiation (GR) drives the mass transfer, and it appears to be the first dynamical evidence that GR is indeed the driver of evolution in this class of very old cataclysmic variables -the AM Canum Venaticorum stars.

Keywords

Accretion, accretion disks; Binaries: close; Novae, cataclysmic variables; Stars: individual (ES Ceti)

Unesco Subjects

21 Astronomía y Astrofísica

Bibliographic citation

Miguel, E. de, Patterson, J., Kemp, J., Myers, G., Rea, R., Krajci, T., Monard, B., & Cook, L. M. (2017). Orbital Period Increase in ES Ceti. In The Astrophysical Journal (Vol. 852, Issue 1, p. 19). American Astronomical Society. https://doi.org/10.3847/1538-4357/aa9ed6

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