A holistic approach to carbon-enhanced metal-poor stars

By T. Masseron, John A. Johnson, B. Plez, S. V. Eck, F. Primas, S. Goriely, A. University, Usa, Graal, U. Montpellier and 7 more. 2009

195 citations recorded by the source corpus.

Context. Carbon-enhanced metal-poor (CEMP) stars are known to have properties that reflect the nucleosynthesis of the first low- and intermediate-mass stars, because most have been polluted by a no ...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a5be4d0e5cf6fd42ae7125e91cc97d2cbf257fd7

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In Astronomy and Astrophysics

1. A. Karakas
2. Timothy C. Beers
3. J. Norris
4. A. Frebel
5. R. Hirschi
6. M. Lugaro
7. Selma de Mink
8. G. Meynet

In Instrumentation

1. Timothy C. Beers
2. A. Karakas
3. A. Frebel
4. R. Hirschi
5. J. Norris
6. Robert G. Izzard
7. M. Lugaro
8. Selma de Mink

Citations in the corpus

• XHIP: An extended hipparcos compilation (2011, unknown): “(2011), Santos et al. (2011), Masseron et al. (2010), Gebran et al. (2010), Schuster (2010), Ramirez et al. (2009), Guillout et al. (2009), Nissen & Jenkins et al. (2008), Soubiran et al. (2008), Robinson et al. (2007), GCS3, Taylor (2005), Soubiran et al. (2003), Beers et al. (2000), and Chiba &…”
• CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, background): “As it is often found that N is enhanced in CEMP stars (Masseron et al. 2010), we assume the same level of N enhancement as for carbon (i.e., [N/Fe] = [C/Fe]).”
• The s-Process in Low Metallicity Stars. II. Interpretation of High-Resolution Spectroscopic Observations with AGB models (2011, methodology): “All stars have metallicities in the range −3.5 6 [Fe/H] 6 −1.7, with five exceptions: CS 29503–010 ([Fe/H] = −1.06; Aoki et al. 2007), HD 26 ([Fe/H] = −1.25,−1.02; Van Eck et al. 2003, Masseron et al. 2010), HD 206983 ([Fe/H] = −0.99, −1.43; Junqueira & Pereira 2001, Masseron et al. 2010), HE 0507–1”
• THE MOST METAL-POOR STARS. IV. THE TWO POPULATIONS WITH [Fe/H] ≲ −3.0 (2012, background): “−3.0 Binarity has been suggested as a necessary or likely explanation for the carbon richness of some or all of the Crich stars (21 CEMP-no stars plus two having [Fe/H]∼ – 5.5) in Table 1 (e.g., Suda et al. 2004; Masseron et al. 2010).”
• Wind Roche-lobe overflow: Application to carbon-enhanced metal-poor stars (2013, background): “Beers & Christlieb (2005) and Masseron et al. (2010) provide detailed reviews of the CEMP subgroups.”
• A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, unknown): “Abundances derived from previous moderate or high resolution spectroscopy of seven of the remaining 25 stars have been presented elsewhere by Norris et al. (1993), Spite et al. (2000), Preston & Sneden (2001), Lai et al. (2004), and T. Masseron et al. (unpublished; see Masseron et al. 2010).”
• s-process production in rotating massive stars at solar and low metallicities (2015, background): “Recent catalogues may be found by Masseron et al. (2010), Allen et al. (2012), Bisterzo et al. (2012), Lugaro et al. (2012), Norris et al. (2013), Bonifacio et al. (2015) and Hansen et al. (2015).”
• CH in stellar atmospheres: an extensive linelist (2014, background): “The elemental abundances are from Masseron et al. (2010) (except for HE 2201-0345, Masseron et al., in prep.).”
• Near-Field Cosmology with Extremely Metal-Poor Stars (2015, unknown): “…Norris et al. (2007), Frebel et al. Lai et al. (2008), Cohen et al. (2008), Meynet et al. (2010), Heger & Woosley (2010), Joggerst et al. (2010), Masseron et al. (2010), Nomoto, Kobayashi & Tominaga (2013), Frebel & Norris (2013), Norris et al. (2013), and Tominaga, Iwamoto & Nomoto (2014) for…”
• Binarity in carbon-enhanced metal-poor stars (2014, background): “Based on their abundance patterns, it has been suggested that the CEMP-r/s class has the same binary origin as the CEMP-s stars (e.g., Masseron et al. 2010; Allen et al. 2012), although this might mean that a different neutron-capture process with features in between the r- and s-process will need…”
• NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “…et al. 2003a) and the spectroscopic observations of stars at different metallicities (Lambert et al. 1995; Busso et al. 2001; Abia et al. 2002; Masseron et al. 2010; Bisterzo et al. 2011; Lugaro et al. 2012; Maiorca et al. 2012) and planetary nebulae (Karakas et al. 2007; Pignatari et al.…”
• THE MOST METAL-POOR STARS. II. CHEMICAL ABUNDANCES OF 190 METAL-POOR STARS INCLUDING 10 NEW STARS WITH [Fe/H] ⩽ −3.5,, (2012, background): “Cohen et al. (2006) and Masseron et al. (2010) have suggested that the CEMP-no stars are likely the extremely metal-poor counterparts of the CEMP-s stars.”
• THE s-PROCESS IN ASYMPTOTIC GIANT BRANCH STARS OF LOW METALLICITY AND THE COMPOSITION OF CARBON-ENHANCED METAL-POOR STARS (2011, methodology): “Figure 5 presents an overview of the observational data for CEMP stars and carbon- normal metal-poor stars of the rI and rII subclasses following the data and classification of Masseron et al. (2010).”
• CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES (2014, unknown): “…Hansen et al. (2011, 2014), Hollek et al. (2011, 2014), Ito et al. (2013), Johnson et al. (2007), Jonsell et al. (2006), Lai et al. (2007, 2008), Masseron et al. (2010), Mashonkina et al. (2012), McWilliam et al. (1995), Meléndez & Barbuy (2002), Placco et al. (2013, 2014b), Preston & Sneden…”