Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars

By T. Bensby, S. Feltzing, I. Lundström. 2003

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View Paper: https://www.semanticscholar.org/paper/46a36fb650a30f65e902a4e16b731bea41d810c7

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In Astronomy and Astrophysics

Citations in the corpus

The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “In Figure 13, the stars of the thick disk are mostly older than those of the thin disk and have a distinct chemistry (Bensby et al. 2003, Haywood 2006, Schuster et al. 2006, Bensby 2014).”
Through thick and thin: kinematic and chemical components in the solar neighbourhood (2010, background): “…older and more highly enriched in α elements than their thin disk counterparts supports the twocomponent nature of the Galactic disk (Gratton et al. 1996; Fuhrmann 1998; Prochaska et al. 2000; Bensby et al. 2003; Gilmore & Wyse 1985; Reddy et al. 2006; Bensby et al. 2007; Fuhrmann 2008).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, methodology): “…et al. 1993; Favata et al. 1997; Fuhrmann 2008) rely on kinematically unbi- ased samples, many investigations (e.g., Feltzing & Gustafsson 1998; Bensby et al. 2003; Reddy et al. 2006; Bensby et al. 2007; Ramı́rez et al. 2007; Soubiran et al. 2008) make use of sophisticated kinematic…”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, background): “For [Fe/H] > −1.0, Al shows a ‘Mglike behaviour’ (Bensby et al. 2003, 2005; Reddy et al. 2006).”
CHEMICAL CARTOGRAPHY WITH APOGEE: METALLICITY DISTRIBUTION FUNCTIONS AND THE CHEMICAL STRUCTURE OF THE MILKY WAY DISK (2015, background): “…2003, 2011; Allende Prieto et al. 2006; Bovy et al. 2012c; Cheng et al. 2012a; Anders et al. 2014), although there do exist thick-disk stars with solar-[α/Fe] abundances and supersolar metallicities (Bensby et al. 2003, 2005, 2014; Adibekyan et al. 2011; Nidever et al. 2014; Snaith et al. 2014).”
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) (2007, positive): “…was the only region for which multiple hundreds or thousands of observations had been assembled for “Galactic field stars” (e.g., Edvardsson et al. 1993, Bensby et al. 2003, Fuhrmann 2004, Venn et al. 2004, Nissen & Schuster 2010, Soubiran et al. 2010, Adibekyan et al. 2012, 2013, Bensby et al.…”
Chemodynamics of the Milky Way - I. The first year of APOGEE data (2013, background): “…the APOGEE and the HARPS sample there is no a-priori reason to expect the observed gap to be caused by selection biases, because unlike in SEGUE, RAVE or the highresolution studies of Bensby et al. (2003) and Ramírez et al. (2013), the thick disc was not targeted preferentially by these surveys.”
Structural Parameters of Thin and Thick Disks in Edge-on Disk Galaxies (2005, background): “They are also significantly enhanced in -elements compared to thin disk stars of comparable iron abundance (Fuhrmann 1998; Prochaska et al. 2000; Tautvaišienė et al. 2001; Bensby et al. 2003; Feltzing et al. 2003; Mishenina et al. 2004; Brewer & Carney 2004; Bensby et al. 2005).”
The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk (2013, background): “Kinematics are also often used to segregate thin and thick disk stars (e.g. Soubiran et al. 2003; Bensby et al. 2003), but have currently offered few insights beyond simple classification, and may even represent a loss of information if it is used to group all the kinematic data.”
INSIDE OUT AND UPSIDE DOWN: TRACING THE ASSEMBLY OF A SIMULATED DISK GALAXY USING MONO-AGE STELLAR POPULATIONS (2013, background): “However, bimodal distributions in vertical star counts (e.g., Gilmore & Reid 1983), kinematics (e.g., Bensby et al. 2003), and chemistry (e.g., Lee et al. 2011) in the solar neighborhood suggest a distinct thick disk.”
A RADIAL AGE GRADIENT IN THE GEOMETRICALLY THICK DISK OF THE MILKY WAY (2016, background): “…the disk midplane (Yoachim & Dalcanton 2008a; Rejkuba et al. 2009; Cheng et al. 2012a); (2) kinematically (Morrison et al. 1990; Majewski 1992; Bensby et al. 2003; Reddy et al. 2003; Adibekyan et al. 2012; Haywood et al. 2013); (3) chemically, as the α-rich sequence in the [α/Fe] versus…”
FUNDAMENTAL PARAMETERS AND CHEMICAL COMPOSITION OF ARCTURUS (2011, background): “These trends separate stars that are members of the so-called Galactic thin disk from those of the thick disk (e.g., Fuhrmann 1998; Bensby et al. 2003; Reddy et al. 2003, 2006).”
A library of high resolution synthetic stellar spectra from 300 nm to 1.8 μm with solar and α-enhanced composition (2005, methodology): “Line by line fits to the solar spectrum were done in specific spectral regions, and in this process ∼ 240 lines had their log gf s selected among values from Sneden et al. (1996), Kupka et al. (1999; VALD), Biehl (1976), Steffen (1985), McWilliam & Rich (1994) and Bensby et al. (2003).”
Galactic Chemical Evolution: Carbon through Zinc (2006, background): “Observational data of thick disk stars are shown (Prochaska et al. 2000; Bensby et al. 2003; Gratton et al. 2003), except for the large stars are for bulge stars (McWilliam & Rich 2004).”
alpha-, r-, and s-process element trends in the Galactic thin and thick disks (2004, methodology): “In Bensby et al. (2003) we compared our solar equivalent widths (measured in a FEROS spectrum) to those in Edvardsson et al. (1993) and found good agreement.”