Learn More
We compare the first direct angular diameter measurements obtained on our closest stellar neighbour, α Centauri to recent model diameters constrained by asteroseismic observations. Using the VINCI instrument installed at ESO's VLT Interferometer (VLTI), the angular diameters of the two main components of the system, α Cen A and B were measured with a(More)
We report the angular diameter measurement obtained with the VINCI/VLTI instrument on the nearby star Procyon A (α CMi A, F5IV-V), at a relative precision of ±0.9 %. We obtain a uniform disk angular diameter in the K band of θUD = 5.376 ± 0.047 mas and a limb darkened value of θLD = 5.448 ± 0.053 mas. Together with the hipparcos parallax, this gives a(More)
Solar models computed with mass loss, microscopic diffusion of helium and heavy element, and with updated physics have been evolved from the pre-main sequence to present day; they are compared to the observational constraints including lithium depletion and to the seismic reference model of Basu et al. (1996), derived by inversion. Microscopic diffusion(More)
We present the work undertaken by the Evolution and Seismic Tools Activity (ESTA) team of the CoRoT Seis-mology Working Group. We have focused on two main tasks: Task 1 – now finished – has aimed at testing, comparing and optimising seven stellar evolution codes which will be used to model the internal structure and evolution of the CoRoT target stars. Task(More)
Visualizations of the leading edge cavity on a four-bladed inducer working with refrigerant 114 are presented. The evolution of the cavity length with the cavitation number is given for three different temperatures. These data are used to estimate the thermodynamic effect in R114. In addition, the onset of cavitation instabilities (alternate blade(More)
Observations of surface oscillations of the Sun can be analyzed to probe the solar interior. We use data obtained by the LOWL instrument (LOWL is an abbreviation for low degree with degree denoted by L) installed on Mauna Loa, Hawaii, since 1994 to investigate solar internal rotation. A 2 Dimensional Regularized Least-Squares (2D RLS) inverse method based(More)