Abstract
We investigate the relativistic effects in the orbital motion of the exoplanet HD 80606b with a high eccentricity of e ≃ 0.93. We propose a method to detect these effects (notably the orbital precession) based on measuring the successive eclipse and transit times of the exoplanet. In the case of HD 80606b, we find that in ten years (after approximately 33 periods) the instants of transits and eclipses are delayed with respect to the Newtonian prediction by about three minutes due to relativistic effects. These effects can be detected by comparing at different epochs the time difference between a transit and the preceding eclipse, and should be measurable by comparing events already observed on HD 80606 in 2010 with the Spitzer satellite together with those to be observed in the future with the James Webb Space Telescope.
Highlights
Whereas more than 4000 exoplanets have been discovered so far, the planet orbiting the G5 star HD 80606 remains a remarkable and unique case
In this paper we propose to detect the general relativistic (GR) precession of the periastron for the exoplanet HD 80606b by using a method based on the transit times, computing a small drift in the successive instants of transits due to relativity
In this paper we investigated the relativistic effects in the orbital motion of the high eccentricity exoplanet HD 80606b orbiting around the G5 star HD 80606
Summary
Whereas more than 4000 exoplanets have been discovered so far, the planet orbiting the G5 star HD 80606 remains a remarkable and unique case. The obliquity of the system could be measured from the Rossiter–McLaughlin anomaly observed during transits, which revealed that the orbit of HD 80606b is prograde but inclined (Moutou et al 2009; Pont et al 2009; Winn et al 2009); Hébrard et al (2011) reported an obliquity of λ = 42◦ ± 8◦. In this paper we propose to detect the GR precession of the periastron (and the relativistic orbital motion) for the exoplanet HD 80606b by using a method based on the transit times, computing a small drift in the successive instants of transits due to relativity. 2 we introduce the geometrical conventions used to compute the times of transits and eclipses Those are computed in two different ways: a post-Keplerian parametrisation of the orbit, and a Hamiltonian method using Delaunay-Poincaré canonical variables in Sect. A quick but rough estimate of the GR shift of transit times is given in Appendix A
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
