Poster abstract details
Determination of dynamical and physical parameters of the system CoRoT 3
Abstract
The two main tools to determine the dynamical and physical parameters of exoplanet systems are the radial velocity (RV) measurements and, when available, transit timings. The two techniques are complementary: The RV's allow us to know some of the orbital elements while the transit timings allow us to obtain the orbital inclination, solving the indetermination of the mass, and planetary radius, impossible of obtain from the RV's.
The space observation of transiting planets is however not limited to transit times. They extend to long periods of time and are precise enough to provide information on variations along the orbit. Besides the effects of stellar rotation, deserve mention the Doppler shift in the radiation flux, or Beaming Effect (BE); the Ellipsoidal Variability (EV) from to the tidal deformation of the star due to the gravitation of its close companion; and the Reflection (ER) of the stellar radiation incident on the planet and re-emitted to the observer. In the case of large hot Jupiters, these effects are enhanced by the strong gravitational interactions and the analysis of the light variation allows us independent estimates of the mass and radius of planet.
The planetary system CoRoT 3 is favorable for such analysis. In this case, the secondary is a brown dwarf whose mass is of the order of \approx 22 M_{J}. We show results obtained from the analysis of 35 RV measurements, 236999 photometric observations and 11 additional RV made during a transit to determine the star rotation via the Rossiter-McLaughlin effect. The results obtained from this determination are presented in this communication and are compared to those from other determinations.
The space observation of transiting planets is however not limited to transit times. They extend to long periods of time and are precise enough to provide information on variations along the orbit. Besides the effects of stellar rotation, deserve mention the Doppler shift in the radiation flux, or Beaming Effect (BE); the Ellipsoidal Variability (EV) from to the tidal deformation of the star due to the gravitation of its close companion; and the Reflection (ER) of the stellar radiation incident on the planet and re-emitted to the observer. In the case of large hot Jupiters, these effects are enhanced by the strong gravitational interactions and the analysis of the light variation allows us independent estimates of the mass and radius of planet.
The planetary system CoRoT 3 is favorable for such analysis. In this case, the secondary is a brown dwarf whose mass is of the order of \approx 22 M_{J}. We show results obtained from the analysis of 35 RV measurements, 236999 photometric observations and 11 additional RV made during a transit to determine the star rotation via the Rossiter-McLaughlin effect. The results obtained from this determination are presented in this communication and are compared to those from other determinations.