The Galactic abundance gradient from Cepheids - V. Transition zone between 10 and 11 kpc

By S. Andrievsky, R. E. Luck, P. Martin, J. Lépine. 2004

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In Astronomy and Astrophysics

Citations in the corpus

Galactic Metallicity Gradients Derived from a Sample of OB Stars (2004, background): “Besides, there may be a discontinuity in the radial Galactic gradient with two distinct metallicity zones in the disk (results from open clusters from Twarog, Ashman, & Anthony-Twarog 1997 and Cepheids by Caputo et al. 2001; Andrievsky et al. 2004).”
On the metallicity of open clusters. III. Homogenised sample (2015, methodology): “The most common results are linear fits over the complete investigated RGC range, as presented for example by Chen et al. (2003), Friel et al. (2002), and many others, but also gradients with different slopes for inner and outer areas were applied (e.g. by Andrievsky et al. 2004; Yong et al. 2012).”
A Spectroscopic Study of the Ancient Milky Way: F- and G-Type Stars in the Third Data Release of the Sloan Digital Sky Survey (2005, result): “These stars also exhibit a flat or very small metallicity variation, in contrast with the marked gradient found in the thin disk from open clusters, Cepheids, H ii regions, or massive stars (e.g., Twarog et al. 1997; Andrievsky et al. 2004; Vı́lchez & Esteban 1996).”
On the fine structure of the Cepheid metallicity gradient in the Galactic thin disk (2014, background): “4) with the possible occurrence either of a change in the slope or of a shoulder for 7≤ RG ≤10 kpc, as suggested by Twarog et al. (1997); Caputo et al. (2001); Andrievsky et al. (2004).”
FORMATION AND EVOLUTION OF THE DISK SYSTEM OF THE MILKY WAY: [α/Fe] RATIOS AND KINEMATICS OF THE SEGUE G-DWARF SAMPLE (2011, result): “Concerning the variation of the MDFs for cuts in theR distance, many previous studies (e.g., Nordström et al. 2004; Holmberg et al. 2007; Andrievsky et al. 2004; Lemasle et al. 2007; Sestito et al. 2008; Magrini et al. 2009) that used open clusters and/or field stars to derive radial metallicity…”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, methodology): “For the comparison with the observations, we use the homogeneous data for nearly 200 classical Cepheid variable stars presented in a series of papersby S. Andrievsky and collaborators (Andrievsky et al. 2002a,b,c; Luck et al. 2003; Andrievsky et al. 2004; Kovtyukh et al. 2005; Luck et al. 2006).”
Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682) (2009, background): “Such a trend is clearly detected not only in OC, but also in field stars (B-stars and Cepheids), H II regions and planetary nebulae20 (see Chiappini et al., 2001; Andrievsky et al., 2004; Yong etal., 2005; Lemasle et al., 2008, for some review of literature data).”
A FIRST CONSTRAINT ON THE THICK DISK SCALE LENGTH: DIFFERENTIAL RADIAL ABUNDANCES IN K GIANTS AT GALACTOCENTRIC RADII 4, 8, AND 12 kpc (2011, background): “Also OB stars (e.g., Daflon & Cunha 2004; Daflon et al. 2004), and Cepheids (e.g., Andrievsky et al. 2004; Yong et al. 2006) have been observed in the outer disk.”
THE LONG-TERM EVOLUTION OF THE GALACTIC DISK TRACED BY DISSOLVING STAR CLUSTERS (2010, background): “All stellar populations, from the oldest (e.g. planetary nebulae; Maciel et al 2006) to the youngest (e.g. Cepheids; Andrievsky et al 2004), exhibit a marked abundance gradient and show evidence of having flattened with cosmic time.”
A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, background): “…using open clusters (e.g., Bragaglia et al. 2008; Magrini et al. 2009; Yong et al. 2012) or Cepheids (e.g., Andrievsky et al. 2002; Luck et al. 2003; Andrievsky et al. 2004; Lemasle et al. 2008); and (iv) in the oxygen abundance gradient of different individual galaxies, such as M 83 (Bresolin et…”
The evolution of the Galactic metallicity gradient from high-resolution spectroscopy of open clusters (2008, methodology): “In particular, Andrievsky et al. (2004) assume that the SFR is a combination of two components: one proportional to the gas surface density, and the other depending upon the relative velocity of the interstellar gas and spiral arms.”
Direct Determination of the Spiral Pattern Rotation Speed of the Galaxy (2005, background): “These concepts are essential to understand the bimodal gradient of abundance of different elements in the disk (Andrievsky et al., 2004).”