Oral comunication
I. Boisse, X. Dumusque, N. C. Santos, M. Oshagh, X. Bonfils, M. Montalto, G. Boué, C. Lovis
Abstract
The photometric and RV techniques, although extremely efficient to detect and characterize planets are however indirect techniques (as well as astrometry).
Phenomena such as stellar pulsation, inhomogeneous convection, spots or magnetic cycles can prevent us from finding planets or they might degrade the parameters estimation (e.g. Boisse et al. 2009, 2011). We will consider the challenges related to the knowledge of stellar activity for the next decade: detect telluric planets in the habitable zone of their stars (from G to M dwarfs, e.g. Dumusque et al. 2011), understand the activity in the low-mass end of M dwarf (on which will focus future projects like SPIRou or CARMENES, Boisse et al. subm.), limit to the sum of different transit observations in order to characterize the atmospheric components (from the ground or with Spitzer or JWST, Boisse et al. in prep., Oshagh et al. in prep.), as well as the methods proposed and used to overcome this issue.
IAU Symposium 293: Formation, detection, and characterization of extrasolar habitable planets
Beijing, China
2012 August
