We present two independent methods for studying the global stellar parameter space (mass M, age, chemical composition X0, Z0) of HD 49933 with seismic data. Using a local minimization and an MCMC algorithm, we obtain consistent results for the determination of the stellar properties: M = 1.1-1.2 M&sun; Age ~ 3.0 Gyr, Z0 ~ 0.008. A description of

Context. The second short run (SRa02) of the CoRoT space mission for asteroseismology was partly devoted to stars belonging to the Mon OB2 association. An intense monitoring has been performed on Plaskett's star (HD 47129) and the unprecedented quality of the light curve allows us to shed new light on this very massive, non-eclipsing binary system

Context. The CoRoT satellite has recently discovered a hot Jupiter that transits across the disc of a F9 main-sequence star called CoRoT-6 with a period of 8.886 days. Aims: We model the photospheric activity of the star and use the maps of the active regions to study stellar differential rotation and the star-planet interaction. Methods: We apply

We present period change rates (dP/dt) for 42 RR Lyrae variables in the globular cluster IC 4499. Despite clear evidence of these period increases or decreases, the observed period change rates are an order of magnitude larger than predicted from theoretical models of this cluster. We find that there is a preference for increasing periods, a

We observed the new X-ray transient, MAXI J0556-332 (ATel #3102, #3103, #3104, #3106, #3110, #3112) with the Faulkes Telescope South on 17 and 18 January 2011 (MJD 55578.4 and 55579.5). On each date, three 200-sec exposures were taken; one each in Bessel V, R, and I bands, totalling six images. The suggested optical counterpart (ATel #3103) was

We report on the discovery of a relation between the stellar mass M* of early-type galaxies (hereafter ETGs), their shape, as parameterized by the Sersic index n, and their stellar mass-to-light ratio M*/L. In a three-dimensional log space defined by these variables, the ETGs populate a plane surface with small scatter. This relation tells us that