Chemical abundances of 22 extrasolar planet host stars

Huang, Chan; Zhao, Gang; Zhang, H. W.; Chen, Y. Q.

doi:10.1111/j.1365-2966.2005.09395.x

Cited by 62 publications

(5 citation statements)

References 27 publications

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“…In comparison, HD 168443 has an average [Fe/H] abundance of 0.06 dex, with a spread in measurements of 0.18 dex between the groups. The maximum value reported was 0.12 dex by Brugamyer et al (2011) while the lowest was -0.06 dex per Huang et al (2005). HD 137759 had reported similar [Fe/H] measurements by 4 groups, where the maximum was 0.13 dex (Sadakane et al 2005;Ecuvillon et al 2006;Gilli et al 2006), minimum was -0.03 dex (Thévenin & Idiart 1999), and average was [Fe/H] = 0.08 dex.…”

Section: A Note On Stellar Abundancesmentioning

confidence: 90%

Limits on Stellar Companions to Exoplanet Host Stars With Eccentric Planets

Kane

Howell

Horch

et al. 2014

ApJ

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Though there are now many hundreds of confirmed exoplanets known, the binarity of exoplanet host stars is not well understood. This is particularly true of host stars which harbor a giant planet in a highly eccentric orbit since these are more likely to have had a dramatic dynamical history which transferred angular momentum to the planet. Here we present observations of four exoplanet host stars which utilize the excellent resolving power of the Differential Speckle Survey Instrument (DSSI) on the Gemini North telescope. Two of the stars are giants and two are dwarfs. Each star is host to a giant planet with an orbital eccentricity > 0.5 and whose radial velocity data contain a trend in the residuals to the Keplerian orbit fit. These observations rule out stellar companions 4-8 magnitudes fainter than the host star at passbands of 692 nm and 880 nm. The resolution and field-of-view of the instrument result in exclusion radii of 0.05-1.4 ′′ which excludes stellar companions within several AU of the host star in most cases. We further provide new radial velocities for the HD 4203 system which confirm that the linear trend previously observed in the residuals is due to an additional planet. These results place dynamical constraints on the source of the planet's eccentricities, constraints on additional planetary companions, and informs the known distribution of multiplicity amongst exoplanet host stars.

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Section: A Note On Stellar Abundancesmentioning

confidence: 90%

Limits on Stellar Companions to Exoplanet Host Stars With Eccentric Planets

Kane

Howell

Horch

et al. 2014

ApJ

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“…The metallicity factor, m, is defined as log m = [Fe/H]. We assume that the elemental abundance ratios for Mg, Si, and other elements of interest vary similarly with [Fe/H] (e.g., [Mg/H] ≈ [Si/H] ≈ [Fe/H]) over the range of metallicities considered here (see Edvardsson et al 1993;Chen et al 2000;Huang et al 2005). When considering the chemical behavior of individual gases, we focus on higher temperatures (800 K and higher), where thermochemical processes are expected to dominate over disequilibrium processes such as photochemistry or atmospheric mixing (e.g., see Visscher et al 2006).…”

Section: Methodsmentioning

confidence: 99%

Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars. Iii. Iron, Magnesium, and Silicon

Visscher

Lodders

Fegley

2010

ApJ

243

224

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We use thermochemical equilibrium calculations to model iron, magnesium, and silicon chemistry in the atmospheres of giant planets, brown dwarfs, extrasolar giant planets (EGPs), and low-mass stars. The behavior of individual Fe-, Mg-, and Si-bearing gases and condensates is determined as a function of temperature, pressure, and metallicity. Our results are thus independent of any particular model atmosphere. The condensation of Fe metal strongly affects iron chemistry by efficiently removing Fe-bearing species from the gas phase. Monatomic Fe is the most abundant Fe-bearing gas throughout the atmospheres of EGPs and L dwarfs and in the deep atmospheres of giant planets and T dwarfs. Mg-and Si-bearing gases are effectively removed from the atmosphere by forsterite (Mg 2 SiO 4 ) and enstatite (MgSiO 3 ) cloud formation. Monatomic Mg is the dominant magnesium gas throughout the atmospheres of EGPs and L dwarfs and in the deep atmospheres of giant planets and T dwarfs. Silicon monoxide (SiO) is the most abundant Si-bearing gas in the deep atmospheres of brown dwarfs and EGPs, whereas SiH 4 is dominant in the deep atmosphere of Jupiter and other gas giant planets. Several other Fe-, Mg-, and Si-bearing gases become increasingly important with decreasing effective temperature. In principle, a number of Fe, Mg, and Si gases are potential tracers of weather or diagnostic of temperature in substellar atmospheres.Subject headings: astrochemistry -planets and satellites: individual (Jupiter) -stars: low-mass, brown dwarfs -stars: individual (Gliese 229B, HD 209458)

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“…Since the composition of stars can be obtained in many cases (e.g. Huang et al, 2005), it seems appropriate to use it as the compositional constraint for the orbiting planets. With this approach, it is not necessary to fix the size of the metallic core, a parameter highly uncertain even for bodies of the Solar System.…”

Section: Introductionmentioning

confidence: 99%