par Chiavassa, Andréa 
;Bigot, Lionel;Thévenin, Frédéric;Collet, Remo;Magic, Zazralt;Asplund, Martin;Jasniewicz, Gerard
Référence Journal of physics. Conference series, 328, 1, 012012
Publication Publié, 2011
;Bigot, Lionel;Thévenin, Frédéric;Collet, Remo;Magic, Zazralt;Asplund, Martin;Jasniewicz, GerardRéférence Journal of physics. Conference series, 328, 1, 012012
Publication Publié, 2011
Article révisé par les pairs
| Résumé : | Convection plays an essential role in the emerging intensity for many stars that will be observed by Gaia. Convective-related surface structures affect the shape, shift, and asymmetry of absorption lines, the photocentric and photometric variability causing bias in Gaia measurements. Regarding the importance of Gaia mission and its goals, it is mandatory to have the best models of the observed stars. 3-D time-dependent hydrodynamical simulations of surface convection are crucial to model the photosphere of late type stars in a very realistic way. These simulations are an important tool to correct the radial velocities and to better estimate the parallaxes and photometric variability. |
