On the correlation of elemental abundances with kinematics among galactic disk stars

By T. Mishenina, C. Soubiran, V. Kovtyukh, S. A. K. A. O. O. Odessa, Observatoire Aquitain des Sciences de l'Univers. 2004

155 citations recorded by the source corpus.

We have performed the detailed analysis of 174 high-resolution spectra of FGK dwarfs obtained with the ELODIE echelle spectrograph at the Observatoire de Haute-Provence. Abundances of Fe, Si and Ni have been determined from equiv- alent widths under LTE approximation, whereas abundances of Mg have been determined under NLTE approximation using equivalent widths of 4 lines and profiles of 5 lines. Spatial velocities with an accuracy better than 1 km s −1 , as well as orbits, have been computed for all stars. They have been used to define 2 subsamples kinematically representative of the thin disk and the thick disk in order to highlight their respective properties. A transition occurs at (Fe/H) = −0.3. Stars more metal-rich than this value have a flat distribution with Zmax < 1 kpc and σW < 20 km s −1 , and a narrow distribution of (α/Fe). There exist stars in this metallicity regime which cannot belong to the thin disk because of their excentric orbits, neither to the thick disk because of their low scale height. Several thin disk stars are identified down to (Fe/H) = −0.80. Their Mg enrichment is lower than thick disk stars with the same metallicity. We confirm from a larger sample the results of Feltzing et al. (2003) and Bensby et al. (2003) showing a decrease of (α/Fe) with (Fe/H) in the thick disk interpreted as the signature of the SNIa which have progressively enriched the ISM with iron. However our data suggest that the star formation in the thick disk stopped when the enrichment was (Fe/H) = −0.30, (Mg/Fe) =+ 0.20, (Si/Fe) =+ 0.17. A vertical gradient in (α/Fe) may exist in the thick disk but should be confirmed with a larger sample. Finally we have identified 2 new candidates of the HR1614 moving group.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1d28ad3e217ec31675ea465486c6e09b54036e0e

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

Citations in the corpus

Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, methodology): “Following the formulation adopted in previous studies (e.g., Mishenina et al. 2004; Bensby et al. 2005; R06), the probability that a star belongs to the component that has a mean V = Vi and a velocity dispersion σV = σVi , based only on the V velocity of the star, is proportional to exp [−(V −…”
THE GENESIS OF THE MILKY WAY'S THICK DISK VIA STELLAR MIGRATION (2010, background): “…RCUK Fellow 4 University of Zagreb, Croatia 5 Department of Physics and Astronomy, McMaster Univer- sity, Hamilton, Ontario, L8S 4M1, Canada 1998; Prochaska et al. 2000; Tautvaǐsienė et al. 2001; Bensby et al. 2003; Feltzing et al. 2003; Mishenina et al. 2004; Brewer 2004; Bensby et al. 2005).”
Structural Parameters of Thin and Thick Disks in Edge-on Disk Galaxies (2005, background): “The abundance patterns of thick and thin disk stars therefore follow parallel, but distinct, sequences on the [ /Fe] versus [Fe/H] plane, with significant overlap in [Fe/H] (most recently, Bensby et al. 2004a; Mishenina et al. 2004; Gratton et al. 2003).”
Nearby stars of the Galactic disc and halo – IV (2008, unknown): “Thus, among others, we refer here to the work of Prochaska et al. (2000), Mashonkina et al. (2003), Mishenina et al. (2004), Bensby et al. (2005), Brewer & Carney (2006), Reddy, Lambert & Allende Prieto (2006), Ramı́rez, Allende Prieto & Lambert (2007) and references therein.11 While the stars of…”
FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, unknown): “(1) Bruntt et al. (2012), (2) Valenti & Fischer (2005), (3) Mishenina et al. (2004), (4) Kovtyukh et al. (2003), (5) this paper: a - VWA (Bruntt et al. 2010), b - Santos et al. (2004), Sousa et al. (2006) and Sousa et al. (2008), c - ROTFIT (Frasca et al. 2003, 2006). reader to the review by…”
Elemental abundance survey of the Galactic thick disc (2005, methodology): “[Our program reproduces the probabilities given by Bensby et al. (2003, 2005) and Mishenina et al. (2004), when their input data are adopted.]”
Exploring the Milky Way stellar disk - A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood (2013, background): “One of the few studies that does claim to have thin disk stars at lower metallicities, reaching [Fe/H] ≈ −1, is Mishenina et al. (2004).”
Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program - Galactic stellar populations and planets (2012, background): “…old (e.g. Bensby et al. 2005; Adibekyan et al. 2011), metal-poor and α-enhanced (Fuhrmann 1998; Prochaska et al. 2000; Feltzing et al. 2003; Mishenina et al. 2004; Reddy et al. 2006; Haywood 2008b, Lee et al. 2011) stars that move in Galactic orbits with a large-scale height and…”
Using chemical tagging to redefine the interface of the Galactic disc and halo (2015, background): “However, there has been some debate as to whether the thin disk actually extends to metallicities as low as [Fe/H] = –1.0 dex (e.g. Mishenina et al. 2004).”
THE SPATIAL STRUCTURE OF MONO-ABUNDANCE SUB-POPULATIONS OF THE MILKY WAY DISK (2011, background): “…& Dalcanton 2005), and metal-poor (compared to the thin-disk components), as well as enhanced in α-elements (Fuhrmann 1998; Prochaska et al. 2000; Tautvaǐsienė et al. 2001; Bensby et al. 2003; Feltzing et al. 2003; Mishenina et al. 2004; Bensby et al. 2005; Reddy et al. 2006; Haywood 2008).”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, methodology): “…assumed conservative U, V,W errors of 2.5 km s−1, as these values are not given for individual stars in the GCS. Membership probabilities (i.e., the probabilities of a star to be a thin disk, thick disk, and halo mem- ber) were computed as in R07 (their Section 3.3; see also Mishenina et al. 2004).”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, result): “However, it is lower than the 25% adopted in Mishenina et al. (2004) who later estimated an expected range of 2-15% with a larger sample size, similar to that found in Kordopatis et al. (2011), and larger than that noted in Reylé & Robin (2001).”
Radial mixing and the transition between the thick and thin Galactic discs (2008, methodology): “We assigned population membership probabilities according to the method of Mishenina et al. (2004) for all the stars in our sample.”
DIRECT IMAGING OF A COLD JOVIAN EXOPLANET IN ORBIT AROUND THE SUN-LIKE STAR GJ 504 (2013, background): “The kinematic velocity of GJ 504 (U=–38.6, V=1.5, W=–18.0; Mishenina et al. 2004) is consistent with thin disk stars, thus providing no tight constraint on the age, but remaining consistent with the young age provided by gyrochronology and chromospheric activity.”