Metallicity measurements using atomic lines in M and K dwarf stars

@article{Woolf2004MetallicityMU,
  title={Metallicity measurements using atomic lines in M and K dwarf stars},
  author={Vincent M. Woolf and George Wallerstein},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2004},
  volume={356},
  pages={963-968}
}
We report the first survey of chemical abundances in M and K dwarf stars using atomic absorption lines in high-resolution spectra. We have measured Fe and Ti abundances in 35 M and K dwarf stars using equivalent widths measured from λ/Δλ≈ 33 000 spectra. Our analysis takes advantage of recent improvements in model atmospheres of low-temperature dwarf stars. The stars have temperatures between 3300 and 4700 K, with most cooler than 4100 K. They cover an iron abundance range of −2.44 < [Fe/H… 

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References

SHOWING 1-10 OF 29 REFERENCES
Abundances in G. Dwarfs.VI. a Survey of Field Stars.
Data are presented for deriving the abundances of the elements in 21 field stars of very nearly solar type. Ironto-hydrogen ratios are obtained from curves of growth for which the ionization
Chemical abundance analysis of Kapteyn's Star
We report spectral chemical abundances for 12 elements in Kapteyn's Star (HD 33793), a subdwarf M star. We use stellar temperature and gravity parameters derived using the recent interferometric
Abundances and Kinematics of Field Halo and Disk Stars. I. Observational Data and Abundance Analysis
We describe observations and abundance analysis of a high-resolution, high signal-to-noise ratio survey of 168 stars, most of which are metal-poor dwarfs. We follow a self-consistent LTE analysis
Abundances for metal-poor stars with accurate parallaxes , I. Basic data
We present element-to-element abundance ratios measured from high dispersion spectra for 150 field subdwarfs and early subgiants with accurate Hipparcos parallaxes (errors <20%). For 50 stars new
TiO and H2O Absorption Lines in Cool Stellar Atmospheres
We compare the structures of model atmospheres and synthetic spectra calculated using different line lists for TiO and water vapor. We discuss the effects of different line list combinations on the
Cooler and Bigger than Previously Thought? Planetary Host Stellar Parameters from the Infrared Flux Method
Effective temperatures and radii for 92 planet-hosting stars as determined from the infrared flux method (IRFM) are presented and compared with those given by other authors using different
M-subdwarfs: spectroscopic classification and the metallicity scale
We present a spectroscopic classification system for M-dwarfs and M-subdwarfs based on quantitative measures of TiO and CaH features in the region 6200 - 7400 Angstroms. Our sample of cool stars
First radius measurements of very low mass stars with the VLTI
We present 4 very low mass stars radii measured with the VLTI using the 2.2m VINCI test instrument. The observations were carried out during the commissioning of the 104-meter-baseline with two
Solar System Abundances and Condensation Temperatures of the Elements
Solar photospheric and meteoritic CI chondrite abundance determinations for all elements are summarized and the best currently available photospheric abundances are selected. The meteoritic and solar
Water vapour in cool dwarf stars
M dwarf spectra beyond 1.35 mum are dominated by water vapour yet terrestrial water vapour makes it notoriously difficult to make accurate measurement of the water vapour bands from ground-based
...
...