Stellar Parameters and Elemental Abundances of Late-G Giants

By Y. Takeda, Bun'ei Sato, D. Murata. 2008

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The properties of 322 intermediate-mass late-G giants (comprising 10 planet-host stars) selected as the targets of the Okayama Planet Search Program, many of which are red-clump giants, were comprehensively investigated by establishing their various stellar parameters (atmospheric parameters, including turbulent velocity fields, metallicity, luminosity, mass, age, projected rotational velocity, etc.), and their photospheric chemical abundances for 17 elements, in order to study their mutual dependence, connection with the existence of planets, and possible evolution-related characteristics. The metallicity distribution of planet-host giants was found to be almost the same as that of non-planet-host giants, making marked contrast to the case of planet-host dwarfs tending to be metal-rich. Generally, the metallicities of these comparatively young (typical age of � 10 9 yr) giants tend to be somewhat lower than those of dwarfs at the same age, and super-metal-rich ([Fe=H] > 0.2) giants appear to be lacking. Apparent correlations were found between the abundances of C, O, and Na, suggesting that the surface compositions of these elements have undergone appreciable changes due to dredge-up of H-burning products by evolution-induced deep

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/35e40cab92b50846a21aa4b9ae2e972333728283

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Citations in the corpus

Do Kepler Superflare Stars Really Include Slowly Rotating Sun-like Stars?—Results Using APO 3.5 m Telescope Spectroscopic Observations and Gaia-DR2 Data (2019, methodology): “…Astrophysical Journal, 876:58 (39pp), 2019 May 1 Notsu et al. The instrumental broadening velocity vip was calculated using the following equation (Takeda et al. 2008): v R 3 10 2 ln 2 , 7ip 5 = ´ ( ) where R(=λ/Δλ) is the wavelength resolution of the observation.”
Precise Radial Velocities of Giant Stars VII. Occurrence Rate of Giant Extrasolar Planets as a Function of Mass and Metallicity (2014, background): “While Pasquini et al. (2007), Takeda et al. (2008) and Mortier et al. (2013) do not find evidence for such a correlation in their samples of G and K giants, Hekker & Meléndez (2007) find indications for a positive correlation between metallicity and planet occurrence rate for K giant stars.”
Chemical similarities between Galactic bulge and local thick disk red giants: O, Na, Mg, Al, Si, Ca, and Ti (2010, background): “analysis of∼180 clump giants by Mishenina et al. (2006), the study of∼300 nearby giants by Luck & Heiter (2007), the survey of ∼380 giants by Hekker & Meléndez (2007), and the analysis of ∼320 giants by Takeda et al. (2008).”
CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER (2011, background): “…the physical properties of stars generally involves comparing an observed temperature indicator (e.g. color) and luminosity (apparent magnitude, bolometric correction and parallax) to theoretical models of stellar evolution (e.g. Nordström et al. 2004; Valenti & Fischer 2005; Takeda et al. 2008).”
REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, result): “Although recent studies confirmed a planet–metallicity correlation around sub-giant stars, a planet–metallicity correlation was not found for giant stars (Takeda et al. 2008; Ghezzi et al. 2010; Maldonado et al. 2013).”
SPECTROSCOPIC ORBITS FOR 15 LATE-TYPE STARS (2016, background): “Takeda et al. (2008) included it in a spectroscopic analysis of the stellar parameters and elemental abundances of late-G giants.”