Accurate fundamental parameters for A-, F- and G-type Supergiants in the solar neighbourhood

@article{Lyubimkov2009AccurateFP,
  title={Accurate fundamental parameters for A-, F- and G-type Supergiants in the solar neighbourhood},
  author={L S Lyubimkov and David L. Lambert and Sergey I. Rostopchin and Tamara M. Rachkovskaya and Dmitry B. Poklad},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2009},
  volume={402},
  pages={1369-1379}
}
The following parameters are determined for 63 Galactic supergiants in the solar neighbourhood: effective temperature T eff ; surface gravity log g; iron abundance log ∈(Fe); microturbulent parameter V t ; mass M/M ⊙ ; age t and distance d. A significant improvement in the accuracy of the determination of log g, and all parameters dependent on it, is obtained through application of van Leeuwen rereduction of the Hipparcos parallaxes. The typical error in the log g values is now ±0.06 dex for… 

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References

SHOWING 1-10 OF 39 REFERENCES

Surface abundances of light elements for a large sample of early B-type stars – II. Basic parameters of 107 stars

Effective temperatures T e f f , surface gravities log g and interstellar extinctions A v are found for 107 B stars. Distances d of the stars, which are based on the derived T e f f , log g and A v

Surface abundances of light elements for a large sample of early B-type stars – IV. The magnesium abundance in 52 stars – a test of metallicity

From high-resolution spectra a non-local thermodynamic equilibrium analysis of the Mg II 4481.2-A feature is implemented for 52 early and medium local B stars on the main sequence (MS). The influence

Supergiant temperatures and linear radii from near‐infrared interferometry

We present angular diameters for 42 Luminosity Class (LC) I stars and 32 LC II stars that have been interferometrically determined with the Palomar Testbed Interferometer. Derived values of radius

Calibration of Strömgren uvby-H$\beta$ photometry for late-type stars – a model atmosphere approach

Context. The use of model atmospheres for deriving stellar fundamental parameters, such as Teff ,l ogg ,a nd [Fe/H], will increase as we find and explore extreme stellar populations where empirical

The Effective Temperature Scale of FGK Stars. I. Determination of Temperatures and Angular Diameters with the Infrared Flux Method

The infrared flux method (IRFM) has been applied to a sample of 135 dwarf and 36 giant stars covering the following regions of the atmospheric parameter space: (1) the metal-rich ([Fe/H] ≳ 0) end

Surface abundances of light elements for a large sample of early B‐type stars – I. Spectral observations of 123 stars; measurements of hydrogen and helium lines; infrared photometry

High-resolution spectral observations of 123 B0–B5 stars in the main sequence evolutionary phase were obtained at two observatories, namely the McDonald Observatory (McDO) and the Crimean

Determination of the temperatures of selected ISO flux calibration stars using the Infrared Flux Method

Eective temperatures for 420 stars with spec- tral types between A0 and K3, and luminosity classes between II and V, selected for a flux calibration of the Infrared Space Observatory, ISO, have been

Surface abundances of light elements for a large sample of early B‐type stars – III. An analysis of helium lines in spectra of 102 stars

Non-local thermodynamic equilibrium analysis of He I lines in spectra of 102 B stars is implemented in order to derive the helium abundance He/H, the microturbulent parameter V t and the projected

A grid of MARCS model atmospheres for late-type stars. I. Methods and general properties

Context. In analyses of stellar spectra and colours, and for the analysis of integrated light from galaxies, a homogeneous grid of model atmospheres of late-type stars and corresponding flux spectra

Quantitative Spectroscopy of Deneb

Context. Quantitative spectroscopy of luminous BA-type supergiants offers a high potential for modern astrophysics. Detailed studies allow the evolution of massive stars, galactochemical evolution,