EDP Sciences
Free Access
Volume 480, Number 2, March III 2008
Page(s) 563 - 571
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361:20079000

A&A 480, 563-571 (2008)
DOI: 10.1051/0004-6361:20079000

Extrasolar planet detection by binary stellar eclipse timing: evidence for a third body around CM Draconis

H. J. Deeg1, B. Ocaña1, 2, V. P. Kozhevnikov3, D. Charbonneau4, F. T. O'Donovan5, and L. R. Doyle6

1  Instituto de Astrofísica de Canarias, C. Via Lactea S/N, 38205 La Laguna, Tenerife, Spain
    e-mail: hdeeg@iac.es
2  Instituto de Radio Astronomía Milimétrica (IRAM), Av. Divina Pastora 7, Núcleo Central, 18012 Granada, Spain
3  Astronomical Observatory, Ural State University, Lenin ave. 51, Ekaterinburg, 620083, Russia
4  Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
5  California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA
6  SETI Institute, 515 N. Whisman Road, Mountain View, CA 94043, USA

(Received 5 November 2007 / Accepted 28 December 2007)

Aims.Our objective is to elucidate the physical process that causes the observed observed-minus-calculated (O-C) behavior in the M4.5/M4.5 binary CM Dra and to test for any evidence of a third body around the CM Dra system.
Methods.New eclipse minimum timings of CM Dra were obtained between the years 2000 and 2007. The O-C times of the system are fitted against several functions, representing different physical origins of the timing variations.
Results.Using our observational data in conjunction with published timings going back to 1977, a clear non-linearity in O-C times is apparent. An analysis using model-selection statistics gives about equal weight to a parabolic and to a sinusoidal fitting function. Attraction from a third body, either at large distance in a quasi-constant constellation across the years of observations or from a body on a shorter orbit generating periodicities in O-C times is the most likely source of the observed O-C times. The white dwarf GJ 630.1B, a proper motion companion of CM Dra, can however be rejected as the responsible third body. Also, no further evidence of the short-periodic planet candidate described by Deeg et al. (2000, A&A, 358, L5) is found, whereas other mechanisms, such as period changes from stellar winds or Applegate's mechanism can be rejected.
Conclusions.A third body, being either a few-Jupiter-mass object with a period of 18.5 $\pm$ 4.5 years or an object in the mass range of 1.5 $M_{\rm jup}$ to 0.1 $M_{\odot}$ with periods of hundreds to thousands of years is the most likely origin of the observed minimum timing behavior.

Key words: stars: individual: CM Dra -- stars: binaries: eclipsing -- eclipses -- stars: planetary systems

© ESO 2008

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.