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(1) Presentation(s)


Mar. 14/03/2017 14:15 Andromede, Bâtiment 11, Etage 3

LAGARDE Nadège (UMR UTINAM, Observatoire de Besançon)
Chemical clocks of stellar populations in the Milky Way


A broad effort is ongoing with large spectroscopic surveys such as APOGEE, ESO-Gaia, RAVE from which stellar parameters, radial velocities and detailed chemical abundances can be measured for CoRoT, Kepler, and K2 targets. In addition, asteroseismic data of red-giants stars observed by the space missions CoRoT and Kepler allow determination of stellar masses, radii, and can be used to determine the position and ages of stars. This association between spectroscopic and asteroseismic constraints provide a new way to understand galactic and stellar evolutions.

To exploit all potential of this combination it would be crucial to develop our approach of synthetic populations. We develop the Besançon Galactic model (Lagarde et al 2017) for which stellar evolution predictions providing the global asteroseismic properties and the surface chemical abundances along the evolution of low- and intermediate-mass stars are included. For the first time, the BGM can explore the effects of an extra-mixing occurring in red-giant stars. These synthetic populations can be compare with the significant large surveys as APOKASC (APOGEE -Kepler) or CoRoTGEE (CoRoT-APOGEE).

We focus on the surface abondances of carbon and nitrogen which are tracers of internal mixing occurring in red-giant stars. In particular we focus on the effects of thermohaline instability on chemical properties as well as on the determination of stellar ages and masses using surface [C/N] abundance ratio. Comparing our simulations with the new APOKASC and CoRoGEE catalogs including C and N surface abundances, we could provide constraints on physics of internal mixing.

We emphasize the usefulness of population synthesis tools to test stellar models and transport processes inside stars. We show that transport processes occuring in red-giant stars should be taken into account in the determination of ages for future Galactic archaeology studies.

Pour plus d'informations, merci de contacter Lebre A.