CLÉS, Code Liégeois d’Évolution Stellaire

Scuflaire, R.; Théado, S.; Montalbán, J.; Miglio, A.; Bourge, P.-O.; Godart, M.; Thoul, Anne; Noels, A.

doi:10.1007/s10509-007-9650-1

Cited by 255 publications

(186 citation statements)

References 33 publications

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“…Stellar models for non-rotating stars were computed with the evolutionary code CLÉS (Code Liégeois d'Évolution Stellaire, Scuflaire et al 2008a). We used the OPAL2001 equation of state (Rogers & Nayfonov 2002;Caughlan & Fowler 1988), with nuclear reaction rates from Formicola et al (2004) for the 14 N(p, γ) 15 O cross-section.…”

Section: Numerical Tools and Model Input Physicsmentioning

confidence: 99%

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

Briquet

Aerts

Baglin

et al. 2011

A&A

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111

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The O9V star HD 46202, which is a member of the young open cluster NGC 2244, was observed by the CoRoT satellite in October/November 2008 during a short run of 34 days. From the very high-precision light curve, we clearly detect β Cep-like pulsation frequencies with amplitudes of ∼0.1 mmag and below. A comparison with stellar models was performed using a χ 2 as a measure for the goodness-of-fit between the observed and theoretically computed frequencies. The physical parameters of our best-fitting models are compatible with the ones deduced spectroscopically. A core overshooting parameter α ov = 0.10 ± 0.05 pressure scale height is required. None of the observed frequencies are theoretically excited with the input physics used in our study. More theoretical work is thus needed to overcome this shortcoming in how we understand the excitation mechanism of pulsation modes in such a massive star. A similar excitation problem has also been encountered for certain pulsation modes in β Cep stars recently modelled asteroseismically.

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Section: Numerical Tools and Model Input Physicsmentioning

confidence: 99%

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

Briquet

Aerts

Baglin

et al. 2011

A&A

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111

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“…The parameters derived for the WASP-50 system can be found in Table 2. To assess the reliability of the deduced physical parameters we performed a stellar evolution modeling based on the code CLES (Scuflaire et al 2008), using as input the stellar density deduced from our MCMC analysis and the effective temperature and metallicity deduced from our spectroscopic analysis. The resulting stellar mass was 0.84 ± 0.05 M , in good agreement with the MCMC result, 0.89 ± 0.08 M .…”

Section: Global Analysismentioning

confidence: 99%

WASP-50 b: a hot Jupiter transiting a moderately active solar-type star

Gillon

Doyle

Lendl

et al. 2011

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We report the discovery by the WASP transit survey of a giant planet in a close orbit (0.0295 ± 0.0009 AU) around a moderately bright (V = 11.6, K = 10) G9 dwarf (0.89 ± 0.08 M , 0.84 ± 0.03 R ) in the Southern constellation Eridanus. Thanks to highprecision follow-up photometry and spectroscopy obtained by the telescopes TRAPPIST and Euler, the mass and size of this planet, WASP-50 b, are well constrained to 1.47 ± 0.09 M Jup and 1.15 ± 0.05 R Jup , respectively. The transit ephemeris is 2 455 558.6120 (±0.0002) + N × 1.955096 (±0.000005) HJD UTC . The size of the planet is consistent with basic models of irradiated giant planets. The chromospheric activity (log R HK = −4.67) and rotational period (P rot = 16.3 ± 0.5 days) of the host star suggest an age of 0.8 ± 0.4 Gy that is discrepant with a stellar-evolution estimate based on the measured stellar parameters (ρ * = 1.48 ± 0.10 ρ , T eff = 5400 ± 100 K, [Fe/H] = −0.12 ± 0.08) which favors an age of 7 ± 3.5 Gy. This discrepancy could be explained by the tidal and magnetic influence of the planet on the star, in good agreement with the observations that stars hosting hot Jupiters tend to show faster rotation and magnetic activity. We measure a stellar inclination of 84 +6 −31 deg, disfavoring a high stellar obliquity. Thanks to its large irradiation and the relatively small size of its host star, WASP-50 b is a good target for occultation spectrophotometry, making it able to constrain the relationship between hot Jupiters' atmospheric thermal profiles and the chromospheric activity of their host stars.

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“…19). Stellar models were computed with cles (Scuflaire et al 2008b), adiabatic frequencies with losc (Scuflaire et al 2008a), and the stability of modes of degree = 0, 1, 2 was investigated with the code mad (Dupret et al 2003). In the case of δ Sct and γ Doradus stars, the nonadiabatic computations included the interaction between convection and pulsation as described by Grigahcène et al (2005).…”

Section: Comparison With Theoretical Predictionsmentioning

confidence: 99%

CoRoT's view of newly discovered B-star pulsators: results for 358 candidate B pulsators from the initial run's exoplanet field data

Degroote¹,

Aerts

Ollivier

et al. 2009

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Context. We search for new variable B-type pulsators in the CoRoT data assembled primarily for planet detection, as part of CoRoT's additional programme. Aims. We aim to explore the properties of newly discovered B-type pulsators from the uninterrupted CoRoT space-based photometry and to compare them with known members of the β Cep and slowly pulsating B star (SPB) classes. Methods. We developed automated data analysis tools that include algorithms for jump correction, light-curve detrending, frequency detection, frequency combination search, and for frequency and period spacing searches. Results. Besides numerous new, classical, slowly pulsating B stars, we find evidence for a new class of low-amplitude B-type pulsators between the SPB and δ Sct instability strips, with a very broad range of frequencies and low amplitudes, as well as several slowly pulsating B stars with residual excess power at frequencies typically a factor three above their expected g-mode frequencies.Conclusions. The frequency data we obtained for numerous new B-type pulsators represent an appropriate starting point for further theoretical analyses of these stars, once their effective temperature, gravity, rotation velocity, and abundances will be derived spectroscopically in the framework of an ongoing FLAMES survey at the VLT.

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CLÉS, Code Liégeois d’Évolution Stellaire

Cited by 255 publications

References 33 publications

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

WASP-50 b: a hot Jupiter transiting a moderately active solar-type star

CoRoT's view of newly discovered B-star pulsators: results for 358 candidate B pulsators from the initial run's exoplanet field data

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