4 juin - 7 juin 2013


Gaia : Quelles perspectives pour la physique stellaire ?

The Gaia satellite will provide measurements of parallaxes, proper motions, spectro-photometry for a billion of stars, radial velocities for 150 millions, and atmospheric parameters for the brightest objects. With parallaxes of 1% relative accuracy for 10 millions stars, distances to numerous open and globular clusters, determination of masses for numerous stars, Gaia will reveal the fine structure of the HR diagram, for all stellar populations and all phases of stellar evolution. Complemented with new advances in asteroseismology, angular diameter measurements, high resolution spectra, large scale spectroscopic surveys as the Gaia ESO Survey, it is an extensive and high quality dataset that will be available to validate internal and atmospheric models of stars, and more generally for stellar physics. With the launch of Gaia due in september, a first release in 2015, this workshop gives the opportunity to review the expected data, available tools and those needed, ideas and information to obtain the best of the scientific exploitation of the Gaia mission.

Scientific Organizing Committee :
Misha Haywood, Corinne Charbonnel, David Katz, Alejandra Recio-Blanco, Céline Reylé, Caroline Soubiran

6th June
14h00-14h30 J. Montalban : Synergy between asteroseismology and the Gaia mission
14h30-14h50 K. Belkacem : On the seismic scaling relations and their potential to provide accurate stellar parameters
14h50-15h10 J.-L. Halbwachs : Improved SB2 orbits for HIP 12081 and HIP 87895
15h10-15h40 B. Plez : Model atmospheres and fundamental stellar parameters
15h40-16h00 M. Dennefeld : Gaia alerts and stellar physics
16h-16h30 Coffee break
16h30-17h00 A. Recio-Blanco : Stellar parameters from Gaia and related spectroscopic surveys
17h00-17h20 C. Guédé : Age-dating stars in the context of the Gaia mission
17h20-17h40 R. Ezzeddine : NLTE Iron abundance of Kepler Red Giant stars
17h40-18h00 W. Chantereau : A better understanding of the origin of muliple populations in globular clusters