THE DISCOVERY AND ANALYSIS OF VERY METAL-POOR STARS IN THE GALAXY

By Timothy C. Beers, N. Christlieb. 2005

924 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/179d3893952b1e7519595a9eb7c403b19a166eaf

How researchers see this paper

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

1. P. Hopkins
2. A. Frebel
3. Timothy C. Beers
4. Jo Bovy
5. Hans-Walter Rix
6. John H. Wise
7. A. Karakas
8. A. Helmi

Citations in the corpus

• Massive AGB models of low metallicity: the implications for the self-enrichment scenario in metal-poor globular clusters (2009, background): “– in the ejecta having C/O>1, the carbon abundance is small ([C/Fe] 0, Table 2), so that the possible observational counterparts can not be looked for among CEMP (carbon enhanced metal poor) stars, defined as stars for which [C/Fe]>1 (Beers and Christlieb 2005).”
• Two populations of metal-free stars in the early Universe (2006, background): “Finally, we consider how metal-poor Galactic halo stars can be accomodated within our theoretical framework (for a recent review see Beers & Christlieb 2005).”
• Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, background): “Among the second-generation stars, low mass ( 1M ) stars have long lifetimes and might be observed as extremely metalpoor (EMP) stars with ½Fe/H 3 (Beers & Christlieb 2005).”
• The first galaxies : assembly, cooling and the onset of turbulence (2008, background): “The discovery of extremely metal-poor stars in the Galactic halo with masses below one solar mass (Christlieb et al. 2002; Frebel et al. 2005; Beers & Christlieb 2005) indicates that this transition occurs at abundances considerably smaller than the solar value.”
• Stellar Abundances for the Galactic Archeology (SAGA) Database — Compilation of the Characteristics of Known Extremely Metal-Poor Stars (2008, methodology): “Thanks to the recent large-scale searches for candidate Very Metal-Poor stars (hereafter VMP, defined by [Fe/H] ≤−2.0 according to the nomenclature of Beers & Christlieb 2005), in particular by the HK survey (Beers et al. 1985; Beers et al. 1992) and by the Hamburg/ESO survey (Christlieb et al.…”
• Rest-frame ultraviolet-to-optical spectral characteristics of extremely metal-poor and metal-free galaxies (2011, background): “There are hundreds of stars whose metallicity in the atmosphere is found to be extremely low Z 1 × 10−5 (= 1/2000 Z⊙) in the halo of the Galaxy (e.g., Beers & Christlieb 2005).”
• A New View of the Dwarf Spheroidal Satellites of the Milky Way from VLT FLAMES: Where Are the Very Metal-poor Stars? (2006, background): “More recently, the HK and the Hamburg/ESO (HES) surveys have yielded a dramatic increase in the number of metalpoor stars known (Beers & Christlieb 2005).”
• Evolution and nucleosynthesis of extremely metal-poor and metal-free low- and intermediate-mass stars - I. Stellar yield tables and the CEMPs (2008, background): “Goswami et al. 2006; Aoki et al. 2006a; Sivarani et al. 2006; alsosee Beers & Christlieb 2005 for an overview of the observations).”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “The first stars in Z-poor environments are expected to be very massive (Bromm & Larson 2004), and hence, the scaling of mass loss with Z affects abundances of the lowest Z stars (Beers & Christlieb 2005, Bromm & Yoshida 2011) polluted by a small number of early SNe.”
• The Frequency of Carbon-enhanced Metal-poor Stars in the Galaxy from the HERES Sample (2006, background): “…star (HERES) survey (Christlieb et al. 2004, hereafter Paper I; Barklem et al. 2005, hereafter Paper II), which presently provides the largest sample of high-resolution spectra available for very metal-poor (VMP) stars ( according to[Fe/H] ≤ 2.0 the nomenclature of Beers & Christlieb 2005).”
• Carbon-enhanced Metal-poor Stars. I. Chemical Compositions of 26 Stars (2006, background): “There are a growing number of CEMP stars with apparent contributions from both the r-process and the s-process, the CEMP-r/s stars (for further discussion of these classes see Beers & Christlieb 2005).”
• Near-Field Cosmology with Extremely Metal-Poor Stars (2015, methodology): “During the past four decades, extensive study has been devoted to the search for extremely metal-poor stars within the halo of the Galaxy, in order to piece together early chemical evolution soon after the Big Bang (see Beers & Christlieb 2005).”
• THE BIRTH OF A GALAXY: PRIMORDIAL METAL ENRICHMENT AND STELLAR POPULATIONS (2010, background): “These first stellar clusters may be connected to stars in the Milky Way halo and nearby dwarf spheroidal (dSph) galaxies, both with a metallicity floor of [Z/H]7 = –4 (Beers & Christlieb 2005; Frebel et al. 2010; Tafelmeyer et al. 2010).”
• Probing the formation of the first low‐mass stars with stellar archaeology (2007, background): “Together with the currently available data, the imminent arrival of large samples of metal-poor stars such as from SEGUE or LAMOST (Beers & Christlieb 2005), and the Southern Sky Survey in the near future, provides an ideal test bed to empirically constrain and possibly differentiate between differe”
• First stars VIII. Enrichment of the neutron-capture elements in the early Galaxy (2007, unknown): “The latter transition corresponds to [Fe/H]≃ −3, i.e. the metallicity range in which all the highly r-process enriched metal-poor stars are have been found so far – the r-II stars as defined by Beers & Christlieb (2005).”
• Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey (2006, background): “Beers and his collaborators (Beers & Christlieb 2005) found about 1000 stars with [Fe/H] −2.0 by visual detection of Ca II H and K lines.”
• Chemical Evolution in Hierarchical Models of Cosmic Structure. I. Constraints on the Early Stellar Initial Mass Function (2005, background): “This paper adopts the terminology of Beers & Christlieb (2005), who label stars according to their [Fe/H] like so: [Fe/H] −2.0 is “very metal poor” (VMP), [Fe/H] −3.0 is “extremely metal-poor” (EMP), [Fe/H] −4.0 is “ultra-metal poor” (UMP), [Fe/H] −5.0 is “hypermetal poor” (HMP), and, should…”