What Are These Blue Metal-Poor Stars?

By G. Preston, C. Sneden. 2000

181 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5ece93c09642e13706f435d0728131cf1906edbb

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

1. S. Aarseth
2. C. Sneden
3. A. Karakas
4. Robert G. Izzard
5. N. Evans II
6. Pavel Kroupa
7. James S. Bullock
8. Timothy C. Beers

In Computational Mechanics

1. H. Perets
2. D. Fabrycky
3. C. Tout
4. O. Pols
5. J. Hurley
6. S. Aarseth
7. C. Sneden
8. C. Clarke

In Instrumentation

1. S. Aarseth
2. C. Sneden
3. Robert G. Izzard
4. J. Simon
5. V. Belokurov
6. M. Geha
7. E. Carretta
8. R. Gratton

Citations in the corpus

• Stellar Abundances for the Galactic Archeology (SAGA) Database — Compilation of the Characteristics of Known Extremely Metal-Poor Stars (2008, background): “…spectroscopic studies that have been conducted (Gilroy et al. 1988; Ryan et al. 1991; McWilliam et al. 1995; Ryan et al. 1996; Fulbright 2000; Preston & Sneden 2000; Burris et al. 2000; Mishenina & Kovtyukh 2001; Aoki et al. 2002; Cohen et al. 2002; Carretta et al. 2002; Johnson 2002; Nissen…”
• Neutron-Capture Elements in the Early Galaxy (2008, background): “However, they have typically lower eccentricities than do normal field binary systems of comparable periods (see figure 19 of Preston & Sneden 2000).”
• A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, methodology): “For these stars, we list the systemic velocity as determined by Preston & Sneden (2000, 2001), Latham et al. (2002), Carney et al. (2003), Sneden et al. (2003), Pourbaix et al. (2004), or Roederer et al. (2014).”
• The Mass of the Milky Way: Limits from a newly assembled set of halo objects (2002, background): “%) of high-latitude A-type stars are not FHB, but rather some (as yet undetermined) mixture of binaries and high-gravity stars (see Preston & Sneden 2000).”
• Unresolved stellar companions with Gaia DR2 astrometry (2020, result): “…our measurements are in agreement with the earlier spectroscopic studies that found a high fraction of binaries amongst the field BSs (e.g. Preston & Sneden 2000; Carney et al. 2001; Carney, Latham & Laird 2005; Jofré et al. 2016; Matsuno et al. 2018) and BSs in star clusters (e.g.…”
• Binarity in carbon-enhanced metal-poor stars (2014, background): “…of their data combined with radial velocity measurements from McClure & Woodsworth (1990); Norris, Ryan & Beers (1997a); Hill et al. (2000); Preston & Sneden (2000, 2001); Aoki et al. (2001, 2002a,b); Sneden, Preston & Cowan (2003); Van Eck et al. (2003); Lucatello et al. (2003); Cohen et…”
• Abundance Variations within Globular Clusters (2004, background): “As a result, virtually all field BSSs are in binary systems (Preston & Sneden 2000).”
• THE QUENCHING OF THE ULTRA-FAINT DWARF GALAXIES IN THE REIONIZATION ERA (2014, background): “In the Galactic halo, Preston & Sneden (2000) find a much higher ratio:NBS/NHB = 4.4.”
• ON THE TRIPLE ORIGIN OF BLUE STRAGGLERS (2009, methodology): “The field BSSs identified by Preston & Sneden (2000) and Carney et al. (2001) are singlelined spectroscopic binaries, so the companions are consiste t with being WDs, and the orbital period distribution is consistent with that expected from mass transfer in evolved binaries.”
• A complete N-body model of the old open cluster M67 (2005, methodology): “This is based on the Preston & Sneden (2000) observations of field blue metal-poor (BMP) stars.”