DP Leo: eclipsing binary with a planet

December 2009 is quite a hot season for exoplanets, I underline this

http://exoplanet.eu/star.php?st=DP+Leo

Paper:

http://www.iop.org/EJ/abstract/2041-8205/708/1/L66

Wikipedia page:

http://en.wikipedia.org/wiki/DP_Leonis

Incidentally I do find it interesting that many of the Wikipedia articles on extrasolar planet host stars are absolutely terrible at describing the stars and rush straight ahead to get to the planets. DP Leonis is the first known eclipsing polar, a system where accretion occurs onto a highly magnetic white dwarf star. As such it has received a lot of study - but the Wikipedia article pretty much totally neglects it.

The good of Wikipedia is that you can add missing informations when others don't. The important thing is to provide verifiable references.

A&A forthcoming:

Quote :

The giant planet orbiting the cataclysmic binary DP Leonis
K. Beuermann, J. Buhlmann, J. Diese, S. Dreizler, F.V. Hessman, T.-O. Husser, G.F. Miller, N. Nickol, R. Pons, D. Ruhr, H. Schmuelling, A.D. Schwope, T. Sorge, L. Ulrichs, D.E. Winget, K.I. Winget
Received: 17 October 2010 / Accepted: 11 November 2010
DOI: 10.1051/0004-6361/201015942

Noticed that. Beuermann is the same who confirmed NN Ser's companion(s).
Just wondering what about QS Vir after Torino 2010 meeting.

The giant planet orbiting the cataclysmic binary DP Leonis
http://arxiv.org/abs/1011.3905

Quote :

Planets orbiting post-common envelope binaries provide fundamental information on planet formation and evolution, especially for the yet nearly unexplored class of circumbinary planets. We searched for such planets in \odp, an eclipsing short-period binary, which shows long-term eclipse-time variations. Using published, reanalysed, and new mid-eclipse times of the white dwarf in DP\,Leo, obtained between 1979 and 2010, we find agreement with the light-travel-time effect produced by a third body in an elliptical orbit. In particular, the measured binary period in 2009/2010 and the implied radial velocity coincide with the values predicted for the motion of the binary and the third body around the common center of mass. The orbital period, semi-major axis, 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 sin(i_c) = 6.1 +/- 0.5 M_J qualifies it as a giant planet. It formed either as a first generation object in a protoplanetary disk around the original binary or as a second generation object in a disk formed in the common envelope shed by the progenitor of the white dwarf. Even a third generation origin in matter lost from the present accreting binary can not be entirely excluded. We searched for, but found no evidence for a fourth body.

Looks like the designations of circumbinary planets are getting standardised...