A list of data for the broadening of metallic lines by neutral hydrogen collisions

By Paul Barklem, N. Piskunov, B. J. O'mara. 2000

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Citations in the corpus

A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, methodology): “When available, we use damping constants from Barklem et al. (2000) and Barklem & Aspelund-Johansson (2005).”
FUNDAMENTAL PARAMETERS AND CHEMICAL COMPOSITION OF ARCTURUS (2011, methodology): “For Arcturus, we adopted a model atmosphere with α-element enhancement ([α/Fe] = +0.4). van der Waals damping constants were adopted from the works by Barklem et al. (2000) and Barklem & Aspelund-Johansson (2005).”
SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, background): “…line list (∼ 85% of the parameters) were from Kurucz (2010b, 2007, 2010c); Davis et al. (1986); Kurucz (1995, 2013, 2009); Raassen & Uylings (1998); Kurucz (2010a, 2008); Palmeri et al. (2000); Barklem et al. (2000); Goldman et al. (1998); Meggers et al. (1975); Barklem & AspelundJohansson (2005).”
A grid of MARCS model atmospheres for late-type stars. I. Methods and general properties (2008, methodology): “Additional significant progress has been made in the calculation of accurate damping constants for strong atomic lines (Anstee & O’Mara 1995; Barklem et al. 2000a) as well as for hydrogen self broadening (Barklem et al. 2000b).”
High-precision abundances of elements in solar twin stars - Trends with stellar age and elemental condensation temperature (2015, background): “Collisional broadening of Cai, Ti i, Cr i, Fei, Feii, and Nii lines caused by neutral hydrogen and helium atoms is based on quantum mechanical calculations (Anstee & O’Mara 1995; Barklem & O’Mara 1998; Barklem et al. 2000; Barklem & Aspelund-Johansson 2005).”
Giants in the Local Region (2007, methodology): “We have used the van der Waals coefficients of Barklem et al. (2000) when available and otherwise computed them from the Unsöld approximation (Unsöld 1938).”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, methodology): “The pressure broadening damping constants adopted are from Barklem et al. (2000) and Barklem & Aspelund-Johansson (2005), but for lines without damping constants computed by them, we used the values obtained from Unsöld’s formula, multiplied by a factor of 3.”
A library of high resolution synthetic stellar spectra from 300 nm to 1.8 μm with solar and α-enhanced composition (2005, methodology): “The cross sections for ionized transitions presented in Barklem et al. (2000) were included in our line list.”
The Distribution of the Elements in the Galactic Disk (2006, methodology): “For damping in the R. E. L. codes we preferentially use the van der Waals coefficients of Barklem et al. (2000) when available and otherwise compute from theUnsöld approximation (Unsöld 1938).”
Improved Laboratory Transition Probabilities for Neutral Chromium and Redetermination of the Chromium Abundance for the Sun and Three Stars (2007, background): “ABO theory calculations have been done for tens of thousands of lines in the wavelength range 2300-13000 Å of elements Li to Ni with a maximum error of about 20% (Barklem & Aspelund-Johansson 2005; Barklem et al. 2000).”
The elemental composition of the Sun - I. The intermediate mass elements Na to Ca (2014, methodology): “We used damping constants for the collisions with neutral H atoms from Anstee & O’Mara (1995), Barklem et al. (2000), and Barklem (2007) where available.”
The Hamburg/ESO R-process enhanced star survey (HERES). II. Spectroscopic analysis of the survey sample (2005, methodology): “Collisional broadening by neutral hydrogen is, where possible, described by the Anstee, Barklem and O’Mara theory (e.g. Anstee & O’Mara 1991, Barklem et al. 2000 and references therein).”
Abundances in a Large Sample of Stars in M3 and M13 (2004, methodology): “We use the damping constants of Barklem et al. (2000), which were calculated on the basis of the theory of Anstee, Barklem, and O’Mara (Barklem et al. 1998), when available.”
Oxygen trends in the Galactic thin and thick disks (2003, methodology): “The width cross-sections are taken from Anstee & O’Mara (1995), Barklem & O’Mara (1997, 1998), and Barklem et al. (1998, 2000).”