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• W1696752810 abstract "In the seismology program, COROT will explore the entire Main Sequence in the Herzprung-Russel diagram, observing stars from about 1M0 to around 20M0. β Cephei stars are a class of pulsating variables of spectral type B0 to B3. They have periods between 2 and 8 hours, and amplitudes from 0.01 to 0.3 magnitudes. Most of them are multiperiodic. Their oscillation modes are long-lived low-order pressure and gravity modes excited through the so-called κ-mechanism. Their oscillation spectrum is sparse, and the frequencies are well-separated. They are slow rotators, and the rotational splitting is generally much smaller than the separation between the frequencies. One of the main targets in the COROT long-runs program is a β Cephei star. Among the stars which will be observed by COROT, the β cephei stars are probably the ones with the simplest internal structure. They have a large convective core surrounded by a radiative envelope, and they have small rotation velocities. Asteroseismic studies of these stars are very useful, since they will give us information about the global parameters of the star, but also about the size of the convective or mixed region, about the microscopic diffusion processes, and about the velocity profile inside the star. In order to interpret the data which will be obtained by COROT, we will need to confront the observed oscillation frequencies to the theoretically predicted ones. Several stellar evolution codes and oscillation codes will be available to the COROT community. Among the tools which have been developed are the codes CLES (Code Liegeois d’evolution stellaire) and OSC (an adiabatic oscillation code). Given the very high precision of the oscillation data which will be obtained, very precise theoretical computations need to be performed. It takes typically several hours to calculate on a PC the evolution of a β-cephei star and to compute the frequencies of its oscillation modes for all the models on the main sequence (about 100 models per sequence). In order to be able to analyze efficiently the data when it will become available, we have built a grid of models of β cephei stars and a table of their oscillation frequencies, using CLES and OSC. CLES (Scuflaire 2005) is a stellar evolution code which includes all the standard physics and the latest updates for the nuclear reaction rates, the opacities, and the chemical composition. It has been extensively tested and compared to other well-known stellar evolution codes such as CESAM, the Aarhus code ASTEC, and others, and it is state-of-the-art. For the models in this database, we have used the standard metal mixture (GN93), the CEFF equation of state, the OPAL opacity tables, and the standard mixing-length theory of convection. The parameters of a sequence of evolution are the mass (M), the hydrogen mass fraction (X), the metallicity (Z), and the overshooting parameter (α). The grid we have computed contains about 8000 sequences of evolution, with values for the mass ranging from 8 to 20M0 with a step of 0.1M0,three values of X (0.60,0.65,0.70), four values of Z (0.010,0.015, 0.020, 0.025), and five values for the overshooting (0,0.05,0.10,0.15,0.20). There are about 100 stellar models on the main sequence for each stellar evolution. For each model on the main sequence, we have computed the low-degree (n<20) frequencies of oscillation for modes of degree l=0,1,2,and 3." @default.
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• W1696752810 date "2006-11-01" @default.
• W1696752810 modified "2023-09-26" @default.
• W1696752810 title "BetaDat: A beta Cephei database" @default.
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