Volume 577, May 2015
|Number of page(s)||11|
|Section||Planets and planetary systems|
|Published online||12 May 2015|
Disentangling 2:1 resonant radial velocity orbits from eccentric ones and a case study for HD 27894⋆
Max-Planck-Institut für Astronomie,
e-mail: email@example.com, firstname.lastname@example.org
2 Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong, PR China
3 Zentrum für Astronomie der Universtät Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
4 Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany
5 Main Astronomical Observatory of NAS of Ukraine, 27 Zabolotnoho str., 03680 Kyiv, Ukraine
6 Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge MA 02138, USA
Received: 11 February 2015
Accepted: 23 March 2015
Context. In radial velocity (RV) observations, a pair of extrasolar planets near a 2:1 orbital resonance can be misinterpreted as a single eccentric planet, if data are sparse and measurement precision insufficient to distinguish between these models.
Aims. Using the Exoplanet Orbit Database (EOD), we determine the fraction of alleged single-planet RV detected systems for which a 2:1 resonant pair of planets is also a viable model and address the question of how the models can be disentangled.
Methods. By simulation we quantified the mismatch arising from applying the wrong model. Model alternatives are illustrated using the supposed single-planet system HD 27894 for which we also study the dynamical stability of near-2:1 resonant solutions.
Results. Using EOD values of the data scatter around the fitted single-planet Keplerians, we find that for 74% of the 254 putative single-planet systems, a 2:1 resonant pair cannot be excluded as a viable model, since the error due to the wrong model is smaller than the scatter. For 187 EOD stars χ2-probabilities can be used to reject the Keplerian models with a confidence of 95% for 54% of the stars and with 99.9% for 39% of the stars. For HD 27894 a considerable fit improvement is obtained when adding a low-mass planet near half the orbital period of the known Jovian planet. Dynamical analysis demonstrates that this system is stable when both planets are initially placed on circular orbits. For fully Keplerian orbits a stable system is only obtained if the eccentricity of the inner planet is constrained to < 0.3.
Conclusions. A large part of the allegedly RV detected single-planet systems should be scrutinized in order to determine the fraction of systems containing near-2:1 resonant pairs of planets. Knowing the abundance of such systems will allow us to revise the eccentricity distribution for extrasolar planets and provide direct constraints for planetary system formation.
Key words: celestial mechanics / planetary systems / techniques: radial velocities / stars: individual: HD 27894
This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at http://www.exoplanets.org
© ESO, 2015
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