- ID:
- ivo://CDS.VizieR/J/A+A/543/A108
- Title:
- Grid of stellar models, asteroseismology
- Short Name:
- J/A+A/543/A108
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The availability of asteroseismic constraints for a large sample of stars from the missions CoRoT and Kepler paves the way for various statistical studies of the seismic properties of stellar populations. We evaluate the impact of rotation-induced mixing and thermohaline instability on the global asteroseismic parameters at different stages of the stellar evolution from the zero age main sequence to the thermally pulsating asymptotic giant branch to distinguish stellar populations.
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- ID:
- ivo://CDS.VizieR/J/A+AS/98/523
- Title:
- Grids of stellar models. II.
- Short Name:
- J/A+AS/98/523
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Continuing the effort to provide a homogeneous base of extensive and accurate grids of stellar models covering a wide range of metallicities we present a new grid of stellar models at metallicity Z = 0.008, roughly corresponding to the Large Magellanic Cloud composition. The models have been computed for 0.8 to 120 solar masses, using up-to-date input physics and the new radiative opacities from Rogers and Iglesias (1992ApJS...79..507R) and Kurucz (1991). Mass loss and moderate core overshooting are taken into account. The resulting HR diagram and the lifetimes in the H-, He-, and C-burning phases as well as some general results on massive stars are discussed and compared with complementary grids, using the same input physics at metallicities Z of 0.020 and 0.001 used by Schaller et al. (1992, Cat. J/A+AS/96/269)
- ID:
- ivo://CDS.VizieR/J/A+AS/101/415
- Title:
- Grids of stellar models III.
- Short Name:
- J/A+AS/101/415
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Stellar evolutionary models with mass loss and moderate overshooting at metallicity Z = 0.004 in the 0.80 to 120 M{sun} range are presented. They complete the set of grids computed with the same up-input physics for Z=0.020 and 0.001 by Schaller et al. (1992, Cat. J/A+AS/96/269), for Z=0.008 by Schaerer et al. (1992A&A...263..129S, Cat. J/A+AS/98/523) and for Z=0.040 by Schaerer et al. (1993, Cat. J/A+AS/102/339).
- ID:
- ivo://CDS.VizieR/J/A+AS/102/339
- Title:
- Grids of stellar models IV
- Short Name:
- J/A+AS/102/339
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The present grid of evolutionary sequences at metallicity Z=0.040, completes the set of grids computed for Z=0.020 and 0.001 by Schaller et al. (1992, Cat. J/A+AS/96/269), Z=0.008 by Schaerer et al. (1992, Cat. J/A+AS/98/523) and Z=0.004 by Charbonnel et al. (1993, Cat. J/A+AS/101/415). The models with mass loss and moderate core overshooting have been computed for 0.8 to 120 M{sun} using up-to-date input physics and the new radiative opacities from Iglesias et al. (1992ApJ...397..717I) and Kurucz (1991).
- ID:
- ivo://CDS.VizieR/J/A+AS/103/97
- Title:
- Grids of stellar models V.
- Short Name:
- J/A+AS/103/97
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Most outputs of massive star evolution critically depend on the mass loss rates. In order to broaden the comparison basis and to illustrate the effects of different mass loss rates, we have computed new sets of models, with initial masses between 12 and 120 M{sun}, and metallicities, Z, between 0.001 and 0.040, with a mass loss rate increased by a factor of two during the phases when the stellar winds are believed to be essentially driven by the radiation pressure. A moderate core-overshooting and the new radiative opacities from Iglesias et al. (1992ApJ...397..717I) and Kurucz (1991) were taken into account. These models complete the homogeneous and extended theoretical database formed by the previous grids of this series, computed by Schaller et al. (1992, Cat. J/A+AS/96/269) for Z=0.020 and Z=0.001, by Schaerer et al. (1992, Cat. J/A+AS/98/523; 1993, Cat. J/A+AS/102/339) for Z=0.008 and Z=0.040 and by Charbonnel et al. (1993, Cat. J/A+AS/101/415) for Z=0.004. This paper closes this series. Of particular interest is the predicted behaviour of metal rich stars such as may be found in the inner regions of our Galaxy. New evolutionary connexions are found, in particular we show that the most massive and metal rich stars may spend a relatively long time as He and N enriched stars and may even end their evolution as white dwarfs.
- ID:
- ivo://CDS.VizieR/J/A+AS/128/471
- Title:
- Grids of stellar models. VII.
- Short Name:
- J/A+AS/128/471
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a new grid of stellar models from 0.8 to 60M_{sun}_ at Z=0.10, with mass loss and moderate overshooting, from the zero age main sequence to either the helium flash (low mass stars), the early AGB phase (intermediate-mass stars or the end of carbon burning (massive stars). The calculations are done with opacities provided by Iglesias & Rogers (1993ApJ...412..752I), completed by those of Alexander & Ferguson (1994ApJ...437..879A) at low temperatures. This grid is a homogeneous extension to very high metallicity of the previous grids published by the Geneva group. It is useful for the study of galactic bulges, elliptical galaxies and eventually quasars. Calculations of stars more massive than 60M_{sun}_ are not presented as these objects lose almost their entire mass during their main sequence phase, and are likely to end their life as white dwarfs.
- ID:
- ivo://CDS.VizieR/J/A+AS/135/405
- Title:
- Grids of stellar models. VIII.
- Short Name:
- J/A+AS/135/405
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present stellar evolutionary models covering the mass range from 0.4 to 1M_{sun}_ calculated for metallicities Z=0.020 and 0.001 with the MHD equation of state (Hummer & Mihalas, 1988ApJ...331..794H, Mihalas et al., 1988ApJ...331..815M, Daeppen et al., 1988ApJ...332..261D). A parallel calculation using the OPAL (Rogers et al., 1996ApJ...456..902R) equation of state has been made to demonstrate the adequacy of the MHD equation of state in the range of 1.0 to 0.8M_{sun}_ (the lower end of the OPAL tables). Below, down to 0.4M_{sun}_, we have justified the use of the MHD equation of state by theoretical arguments and the findings of Chabrier & Baraffe (1997A&A...327.1039C). We use the radiative opacities by Iglesias & Rogers (1996ApJ...464..943I), completed with the atomic and molecular opacities by Alexander & Fergusson (1994ApJ...437..879A). We follow the evolution from the Hayashi fully convective configuration up to the redgiant tip for the most massive stars, and up to an age of 20Gyr for the less massive ones. We compare our solar-metallicity models with recent models computed by other groups and with observations.
- ID:
- ivo://CDS.VizieR/J/A+A/635/A6
- Title:
- HD 219134 light and RV curves and code
- Short Name:
- J/A+A/635/A6
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- By analysing the transit light-curve of a planet-hosting star or the induced radial velocity oscillations, many useful information on the planet may be retrieved. However, inferring the physical parameters of the planet (mass, size, semi-major axis, etc.) requires the preliminary knowledge of some parameters of the host star, especially its mass and/or radius, that are generally inferred through theoretical evolutionary models. The paper aims at presenting and testing a whole algorithm devoted to the complete characterization of an exoplanetary system thanks to the global analysis of photometric and/or radial velocity time-series combined to observational stellar parameters derived either from spectroscopy or photometry. We developed an integrated tool called MCMCI that combines the Markov Chain Monte Carlo (MCMC) approach for analysing photometric and/or radial velocity time-series with a proper interpolation within stellar evolutionary isochrones and tracks (known as Isochrone placement) to be performed at each chain step, to retrieve stellar theoretical parameters, such as age, mass and radius. We tested the MCMCI both on the HD 219134 multiplanetary system hosting two transiting rocky super-Earths and on WASP-4, that hosts a bloated hot Jupiter. Even considering different input approaches, a final convergence was reached within the code, we found good agreement with the results already stated in the literature and we obtained more precise output parameters, especially concerning planetary masses. The MCMCI tool offers the opportunity of performing an integrated analysis of an exoplanetary system, without splitting it into the preliminary stellar characterization through theoretical models, but rather favouring a close interaction between the light-curve analysis and the isochrones, so that the parameters recovered at each step of the MCMC enter as input of the Isochrone placement.
- ID:
- ivo://CDS.VizieR/J/A+AS/135/555
- Title:
- Illuminated atmospheres limb-darkening coeff. 1.
- Short Name:
- J/A+AS/135/555
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In Table 1 we present the bolometric and monochromatic limb-darkening coefficients for 196 different combinations of the parameters: T_eff (illuminated model's effective temperature), F_rel (relative incident flux, defined in Sect. 2.1), nu (the cosine of the incidence angle relative to the atmosphere normal), T_h (the effective temperature of the illuminating flux). We present coefficients for the linear, quadratic, cubic, logarithmic, and square root laws, together with the quality factor Q (see Sect. 2.2) of the fitting. In Table 2 we present the passband-specific limb-darkening coefficients. We present the coefficients for the Stroemgren uvby filters and for the Johnson-Morgan UBVRI filters. B2 and B3 are the response function of the B filter with and without the earth's atmosphere transmission function, respectively (see Buser R. 1998A&A....62..411B) In Table 3 we give the polynomial coefficients (Eqs. 8-11) for the Stroemgren uvby filters and for the Johnson-Morgan UBVRI filters and the five limb-darkening laws analysed.
- ID:
- ivo://CDS.VizieR/J/A+A/448/181
- Title:
- IR colours of AGB and post-AGB stars
- Short Name:
- J/A+A/448/181
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- With the advent of space missions, like SPITZER and ASTRO-F, with sensitive detectors in the near- and mid-infrared covering a reasonable field-of-view and having a good spatial resolution it will be possible to detect individual AGB stars in Local Group galaxies. The filters used by these missions are non-standard and different from mission to mission. In this paper the colours of mass-losing AGB and post-AGB stars are calculated in the broad-band filters of the SPITZER and ASTRO-F missions, as well as Bessell V,I and 2MASS J,H,K to connect these results to existing ground-based data. The models are calculated for carbon- and oxygen-rich chemistry and cover different effective temperatures and dust compositions.
