Showing results 41 to 50 of 50
   First asteroseismic results from CoRoT; ; et al in Communication in Asteroseismology (2008), 157 About one year after the end of the first observational run and six months after the first CoRoT data delivery, we comment the data exploitation progress for different types of stars. We consider first ... [more ▼] About one year after the end of the first observational run and six months after the first CoRoT data delivery, we comment the data exploitation progress for different types of stars. We consider first results to illustrate how these data of unprecedented quality shed a new light on the field of stellar seismology. [less ▲] Detailed reference viewed: 3 (2 ULg) Two-scale mass-flux closure models for turbulence: p-mode amplitudes in solar-like starsBelkacem, Kevin  ; ; et alin Communications in Asteroseismology (2007), 150 A new closure model has been developed, which takes into account both the skewness of the velocity distribution induced by the presence of two flows in the convection zone, and the effects of turbulence ... [more ▼] A new closure model has been developed, which takes into account both the skewness of the velocity distribution induced by the presence of two flows in the convection zone, and the effects of turbulence onto each flow (Belkacem et al. 2006a). Applied to the formalism of p-mode excitation, it has been possible to validate this theoretical model by a comparison with the observational excitation rates in the solar case using GOLF data (see Belkacem et al. 2006b). The next step is to consider alpha Cen A for which observations of the mode-damping rates are available. [less ▲] Detailed reference viewed: 6 (1 ULg)Solar-like oscillation amplitudes and line-widths as a probe for turbulent convection in stars; Belkacem, Kevin ; et alin IAU Symposium (2007, May 01) Excitation of solar-like oscillations is attributed to turbulent convection and takes place at the upper-most part of the outer convective zones. Amplitudes of these oscillations depend on the efficiency ... [more ▼] Excitation of solar-like oscillations is attributed to turbulent convection and takes place at the upper-most part of the outer convective zones. Amplitudes of these oscillations depend on the efficiency of the excitation processes as well as on the properties of turbulent convection. We present past and recent improvements on the modeling of those processes. We show how the mode amplitudes and mode line-widths can bring information about the turbulence in the specific cases of the Sun and Alpha Cen A. [less ▲] Detailed reference viewed: 2 (1 ULg)The Seismology Programme of CoRoT; ; et al in Proceedings of "The CoRoT Mission Pre-Launch Status - Stellar Seismology and Planet Finding (2006, November 01) 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 CoRoT Seismology Working ... [more ▼] 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 CoRoT Seismology Working Group. With a few illustrative examples, we show how CoRoT data will help to address various problems associated with present open questions of stellar structure and evolution. [less ▲] Detailed reference viewed: 46 (34 ULg)Rotational Splittings with CoRoT, Expected Number of Detections and Measurement Accuracy; ; et al in ESA Special Publication (2006, November 01) One of the main goal of the CoRoT experiment is to determine the internal rotation of stars. A seismic measure of rotation requires the detection and an accurate measurement of rotational splittings. Our ... [more ▼] One of the main goal of the CoRoT experiment is to determine the internal rotation of stars. A seismic measure of rotation requires the detection and an accurate measurement of rotational splittings. Our ability to achieve this goal with CoRoT observations depends on the properties of the target star (in short: spectral type and distance) and will be discussed. [less ▲] Detailed reference viewed: 6 (1 ULg)Why Bothering to Measure Stellar Rotation with CoRoT?; ; et al in ESA Special Publication (2006, November 01) One important goal of the CoRoT experiment is to obtain information about the internal rotation of stars, in particular the ratio of central to surface rotation rates. This will provide constraints on the ... [more ▼] One important goal of the CoRoT experiment is to obtain information about the internal rotation of stars, in particular the ratio of central to surface rotation rates. This will provide constraints on the modelling of transport mechanisms of angular momentum acting in radiative (rotationally induced turbulent) and convective zones (plumes, extension beyond convectively instable regions). Relations between the surface rotation period and age, magnetic activity, mass loss and other stellar characteristics can also be studied with a statistically significant set of data as will be provided by Corot. We present various theoretical efforts performed over the past years in order to develope the theoretical tools which will enable us to study rotation with Corot. [less ▲] Detailed reference viewed: 9 (1 ULg)Theoretical damping rates and phase-lags for solar-like oscillationsDupret, Marc-Antoine ; ; et alin Proceedings of SOHO 18/GONG 2006/HELAS I, Beyond the spherical Sun (2006, October 01) Not Available Detailed reference viewed: 10 (2 ULg)A non-local MLT treatment fitting 3D simulationsDupret, Marc-Antoine ; ; et alin Proceedings of SOHO 18/GONG 2006/HELAS I, Beyond the spherical Sun (2006, October 01) Not Available Detailed reference viewed: 8 (1 ULg)Non-local time-dependent treatments of convection in A-G type starsDupret, Marc-Antoine ; ; et alin Communications in Asteroseismology (2006), 147 Time-Dependent Convection (TDC) models obtained by combining the local treatment of Gabriel (1996) and Grigahcene et al. (2005) and the non-local prescriptions of Spiegel (1963) are presented. We show ... [more ▼] Time-Dependent Convection (TDC) models obtained by combining the local treatment of Gabriel (1996) and Grigahcene et al. (2005) and the non-local prescriptions of Spiegel (1963) are presented. We show that in the stationary unperturbed case, these non-local treatments can be constrained by the results of 3D hydrodynamic simulations (Stein & Nordlund 1998). We consider here the case of solar-type stars with a large convective envelope and A-F type stars with two very thin surface convection zones. [less ▲] Detailed reference viewed: 9 (1 ULg)Asteroseismology of delta Scuti Stars: Problems and Prospects; Dupret, Marc-Antoine ; et alin Journal of Astrophysics & Astronomy (2005), 26 We briefly outline the state-of-the-art seismology of delta Scuti stars from a theoretical point of view: why is it so difficult a task? The recent theoretical advances in the field that these ... [more ▼] We briefly outline the state-of-the-art seismology of delta Scuti stars from a theoretical point of view: why is it so difficult a task? The recent theoretical advances in the field that these difficulties have influenced are also discussed. [less ▲] Detailed reference viewed: 10 (2 ULg) |
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