Volume 553, May 2013
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||25 April 2013|
CoRoT 101186644: A transiting low-mass dense M-dwarf on an eccentric 20.7-day period orbit around a late F-star⋆
Discovered in the CoRoT lightcurves
School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of
Exact Sciences, Tel Aviv University,
2 Observatoire de l’Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
3 Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
4 Universidad de La Laguna, Dept. de Astrofísica, 38200 La Laguna, Tenerife, Spain
5 Institut d’Astrophysique de Paris, UMR 7095, CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France
6 Observatoire de Haute Provence, CNRS/OAMP, 04870 St. Michel l’Observatoire, France
7 Institute of Planetary Research, German Aerospace Centre, Rutherfordstrasse 2, 12489 Berlin, Germany
8 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, 13388 Marseille, France
9 Research and Scientific Support Department, ESTEC/ESA, Keplerlaan 1, 2200 AG Noordwijk, The Netherlands
10 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Received: 6 December 2012
Accepted: 6 February 2013
We present the study of the CoRoT transiting planet candidate 101186644, also named LRc01_E1_4780. Analysis of the CoRoT lightcurve and the HARPS spectroscopic follow-up observations of this faint (mV = 16) candidate revealed an eclipsing binary composed of a late F-type primary (Teff = 6090 ± 200 K) and a low-mass, dense late M-dwarf secondary on an eccentric (e = 0.4) orbit with a period of ~20.7 days. The M-dwarf has a mass of 0.096 ± 0.011 M⊙, and a radius of 0.104-0.006+0.026 R⊙, which possibly makes it the smallest and densest late M-dwarf reported so far. Unlike the claim that theoretical models predict radii that are 5–15% smaller than measured for low-mass stars, this one seems to have a radius that is consistent and might even be below the radius predicted by theoretical models.
Key words: planetary systems / stars: individual: CoRoT 101186644 / binaries: eclipsing / techniques: photometric / techniques: radial velocities
Based on observations made with the 1-m telescope at the Wise Observatory, Israel, the Swiss 1.2-m Leonhard Euler telescope at La Silla Observatory, Chile, the IAC-80 telescope at the Observatory del Teide, Canarias, Spain, and the 3.6-m telescope at La Silla Observatory (ESO), Chile (program 184.C-0639).
© ESO, 2013
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