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Abstract: Planets orbiting post-common envelope binaries provide fundamentalinformation on planet formation and evolution, especially for the yet nearlyunexplored class of circumbinary planets. We searched for such planets in \odp,an eclipsing short-period binary, which shows long-term eclipse-timevariations. Using published, reanalysed, and new mid-eclipse times of the whitedwarf in DP\,Leo, obtained between 1979 and 2010, we find agreement with thelight-travel-time effect produced by a third body in an elliptical orbit. Inparticular, the measured binary period in 2009-2010 and the implied radialvelocity coincide with the values predicted for the motion of the binary andthe third body around the common center of mass. The orbital period, semi-majoraxis, and eccentricity of the third body are P c = 28.0 +- 2.0 yrs, a c = 8.2+- 0.4 AU, and e c = 0.39 +- 0.13. Its mass of M c sini c = 6.1 +- 0.5 M Jqualifies it as a giant planet. It formed either as a first generation objectin a protoplanetary disk around the original binary or as a second generationobject in a disk formed in the common envelope shed by the progenitor of thewhite dwarf. Even a third generation origin in matter lost from the presentaccreting binary can not be entirely excluded. We searched for, but found noevidence for a fourth body.



Author: K. Beuermann, J. Buhlmann, J. Diese, S. Dreizler, F.V. Hessman, T.-O. Husser, G.-F. Miller, N. Nickol, R. Pons, D. Ruhr, H. Schmu

Source: https://arxiv.org/







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