H-alpha and H-beta line profiles of Be stars

Fontaine, G.; Villeneuve, B.; Landstreet, J. D.; Taylor, R. H.

doi:10.1086/190797

Cited by 31 publications

(38 citation statements)

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“…Note that this distance agrees fairly well with d HIPP = 207 +40 −29 pc obtained from the parallax measured by the Hipparcos satellite. , Fontaine et al (1982), Lacy (1977), Hanuschik et al (1995), Hummel et al (1995), Peters (1987Peters ( , 1988aPeters ( ,b,c, 1989aPeters ( ,b, 1990Peters ( , 1991bPeters ( ,c, 1992Peters ( , 1994, Slettebak & Reynolds (1978) and this paper.…”

Section: Fundamental Parameters Of 66 Ophmentioning

confidence: 60%

Variability and pulsations in the Be star 66 Ophiuchi

Floquet

Neiner

Janot-Pacheco

et al. 2002

A&A

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Section: Fundamental Parameters Of 66 Ophmentioning

confidence: 60%

Variability and pulsations in the Be star 66 Ophiuchi

Floquet

Neiner

Janot-Pacheco

et al. 2002

A&A

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“…This code was originally written by Martin Schwarzschild, but has been modified and updated by many astronomers (Montgomery 1998, and references therein). The equation of state for the core of our models is from Lamb (1974) and for the envelopes from Fontaine, Graboske & van Horn (1977). We used the updated opacity OPAL tables (Iglesias & Rogers 1996), neutrino rates of Itoh et al (1996), and ML2/α = 0.6 mixing length theory of Bohm & Cassinelli (1971).…”

Section: Calculating the Modelsmentioning

confidence: 99%

Seismological studies of ZZ Ceti stars - I. The model grid and the application to individual stars

Castanheira¹,

Kepler²

2008

Monthly Notices of the Royal Astronomical Society

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We calculate and explore an extensive adiabatic model grid for pulsating white dwarfs with hydrogen‐dominated atmospheres, the ZZ Ceti stars. We also compared the computed modes with the observed ones for five ZZ Ceti stars that are a representative sample of the whole class of pulsators. We describe our new approach for seismological studies, using the relative observed amplitudes to give weights for the periods in the fit and the external mass and temperature determinations as a guide. Our seismological study is clear evidence that seismology is indeed a powerful tool in the study of stellar structure and evolution.

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“…The equation of state is determined by minimization of a model free energy (see, e.g. Fontaine, Graboske & van Horn 1977) that includes contributions from internal states of the H 2 molecule and all the ionization states of H, He, C, N, O and Mg. Electron degeneracy is included by the method of Eggleton, Faulkner & Flannery (1973). Coulomb and quantum corrections to the equation of state follow the prescription of Iben, Fujimoto & MacDonald (1992), with the Coulomb free energy updated to use the results of Stringfellow, Dewitt & Slattery (1990).…”

Section: Library Of Stellar Interiorsmentioning

confidence: 99%

Synthetic stellar populations: single stellar populations, stellar interior models and primordial protogalaxies

Jiménez

MacDonald

Dunlop

et al. 2004

Monthly Notices of the Royal Astronomical Society

121

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We present a new set of stellar interior and synthesis models for predicting the integrated emission from stellar populations in star clusters and galaxies of arbitrary age and metallicity. This work differs from existing spectral synthesis codes in a number of important ways, namely (1) the incorporation of new stellar evolutionary tracks, with sufficient resolution in mass to sample rapid stages of stellar evolution; (2) a physically consistent treatment of evolution in the Hertzsprung–Russell (HR) diagram, including the approach to the main sequence and the effects of mass loss on the giant and horizontal branch phases. Unlike several existing models, ours yield consistent ages when used to date a coeval stellar population from a wide range of spectral features and colour indexes. We use Hipparcos data to support the validity of our new evolutionary tracks. We rigorously discuss degeneracies in the age–metallicity plane and show that inclusion of spectral features blueward of 4500 Å suffices to break any remaining degeneracy and that with moderate S/N spectra (10 per 20‐Å resolution element) age and metallicity are not degenerate. We also study sources of systematic errors in deriving the age of a single stellar population and conclude that they are not larger than 10–15 per cent. We illustrate the use of single stellar populations by predicting the colours of primordial protogalaxies and show that one can first find them and then deduce the form of the initial mass function (IMF) for the early generation of stars in the Universe. Finally, we provide accurate analytic fitting formulae for ultrafast computation of colours of single stellar populations.

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H-alpha and H-beta line profiles of Be stars

Cited by 31 publications

References 0 publications

Variability and pulsations in the Be star 66 Ophiuchi

Variability and pulsations in the Be star 66 Ophiuchi

Seismological studies of ZZ Ceti stars - I. The model grid and the application to individual stars

Synthetic stellar populations: single stellar populations, stellar interior models and primordial protogalaxies

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