Searching for Planets in the Hyades. IV. Differential Abundance Analysis of Hyades Dwarfs

By D. Paulson, C. Sneden, W. Cochran. 2003

139 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/d5a759881c4d654523708868224cb15bdcd02262

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Exploring the Frequency of Close-in Jovian Planets around M Dwarfs (2006, background): “They should have a similar metal content to the cluster mean of ½Fe/H ¼ 0:13 0:01 (Paulson et al. 2003).”
Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682) (2009, unknown): “Ramı́rez & Cohen (2003),vt = 4.08 − 5.01 10−4 Teff, and of Carretta et al. (2004),vt = 1.5− 0.13 logg.”
A Planetary Companion to the Hyades Giant ϵ Tauri (2007, background): “Perryman et al. (1998) derived a mean metallicity for the Hyades of ½Fe/H ¼ 0:14 0:05 from the compiled data of 40 Hyades stars, and Paulson et al. (2003) reported acluster mean ½Fe/H ¼ 0:13 0:01 based on high-resolution spectra of FYK dwarfs.”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, methodology): “This value is slightly lower than the mean obtained using the same stars in Paulson et al. (2003), which amounts to [Fe/H] = 0.14± 0.01 dex (σ = 0.04 dex) and nearly coincides with the mean value derived by Paulson et al. (2003) using a larger sample of cluster members.”
Low-Mass Dwarf Template Spectra from the Sloan Digital Sky Survey (2006, methodology): “Metallicity: Spectral Features We explored the effects of metallicity on the spectra by comparing our composite templates to a low-metallicity subdwarf (½Fe/H 0:5; Woolf & Wallerstein 2006) and a metal-rich Hyades dwarf (½Fe/H ¼ 0:13; Paulson et al. 2003), both observed with SDSS.”
The evolution of the Galactic metallicity gradient from high-resolution spectroscopy of open clusters (2008, unknown): “The numbers of stars used in each analysis range from 1 to 15, with the exception of the very rich set by Paulson et al. (2003) for the Hyades (55 dwarf stars).”
Abundances of Baade’s Window Giants from Keck HIRES Spectra. I. Stellar Parameters and [Fe/H] Values (2005, background): “Boesgaard & Friel (1990) and Paulson et al. (2003) studied solar-type Hyades dwarfs (which avoids many of the analysis problems encountered here) and found mean [Fe/H] values of +0:127 0:022 and 0:13 0:01, respectively.”
Detection Limits from the McDonald Observatory Planet Search Program (2006, methodology): “…2002; Kürster et al. 2003), and a program to use the Keck 1 HIRES spectrograph to search for planetary companions to stars in the Hyades (Cochran et al. 2002; Paulson et al. 2002, 2003, 2004a,b) and in the use of the High Resolution Spectrograph on the Hobby-Eberly Telescope (Cochran et al. 2004).”