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The magnetic field of the B3V star 16 Pegasi
H. F. Henrichs, C. Neiner, R. S. Schnerr +8
The Slowly Pulsating B3V star 16 Pegasi was discovered by Hubrig (2006) to be magnetic, based on low-resolution spectropolarimetric observations with FORS1 at the VLT. We have conf…
The MiMeS Project: First Results
J. H. Grunhut, E. Alecian, D. A. Bohlender +11
Massive stars are those stars with initial masses above about 8 times that of the sun, eventually leading to catastrophic explosions in the form of supernovae. These represent the…
The seismology programme of CoRoT
E. Michel, A. Baglin, M. Auvergne +1
We introduce the main lines and specificities of the CoRoT Seismology Core Programme. The development and consolidation of this programme has been made in the framework of the CoRo…
The Gaia satellite: a tool for Emission Line Stars and Hot Stars
Christophe Martayan, Yves Fremat, Ronny Blomme +19
The Gaia satellite will be launched at the end of 2011. It will observe at least 1 billion stars, and among them several million emission line stars and hot stars. Gaia will provid…
Radial velocities, dynamics of stars and nebulosities with GAIA and VLT-GIRAFFE
Christophe Martayan, Yves Fremat, Ronny Blomme +8
This document is divided in two parts. The first part deals with the radial velocities (RV) distributions for B-type stars and nebulosities observed with the VLT-GIRAFFE in the Lar…
Variability of B and Be stars in the LMC/SMC: binaries and pulsations
Christophe Martayan, Pascual Diago, Juan Gutiérrez-Soto +5
To study the variability of the 523 B and Be stars observed in the Magellanic clouds with the VLT-FLAMES, we cross-matched the stars of our sample with the photometric database MAC…
Early-type objects in NGC6611 and Eagle Nebula
Christophe Martayan, Michele Floquet, Anne-Marie Hubert +4
An important question about Be stars is whether Be stars are born as Be stars or not. It is necessary to observe young clusters to answer this question. Observations of stars in NG…