Parent Stars of Extrasolar Planets. V. HD 75289

Abstract

The results of a new spectroscopic analysis of HD 75289, recently reported to harbor a Jovian-mass planet, are presented. From high-resolution, high-S/N ratio spectra, we derive [Fe/H] = +0.28 ± 0.05 for this star, in agreement with the spectroscopic study of Gratton et al., published 10 years ago. In addition, we present a re-analysis of the spectra of υ And and τ Boo; our new parameters for these two stars are now in better agreement with photometrically-derived values and with the recent spectroscopic analyses of Fuhrmann et al. We also report on extended abundance analyses of 14 Her, HD 187123, HD 210277, and ρ 1 Cnc.If we include the recent spectroscopic analyses of HD 217107 by Randich et al. and Sadakane et al., who both reported [Fe/H] ∼ +0.30 for this star, we can state that all the "hot-Jupiter" systems studied to date have metal-rich parent stars. We find that the mean [C/Fe] and [Na/Fe] values among the stars-with-planets sample are smaller than the corresponding quantities among field stars of the same [Fe/H].

Evidence for a Very Young Age of F Stars with Extrasolar Planets

“…Therefore, an age of about the Hyades or younger appears to be quite consistent with the combined data for these three stars. Finally, the age of HD 120136 (t Boo) appears in Figure 4 as ∼1.5 Gyr and is within the range given by other authors (see Gonzalez & Laws 2000;Henry et al 2000). The actual age is probably younger because the uvby data apparently underestimate the metallicity of this star (compare 0.14 dex with 0.32 dex from the spectroscopic analysis in Gonzalez & Laws 2000), which overestimates its age from isochrone fitting.…”

“…Finally, the age of HD 120136 (t Boo) appears in Figure 4 as ∼1.5 Gyr and is within the range given by other authors (see Gonzalez & Laws 2000;Henry et al 2000). The actual age is probably younger because the uvby data apparently underestimate the metallicity of this star (compare 0.14 dex with 0.32 dex from the spectroscopic analysis in Gonzalez & Laws 2000), which overestimates its age from isochrone fitting. In addition, t Boo is characterized by low variability, DHp p The combined evidence from the above analysis suggests that the PB F stars considered here are very young, about the age of the Hyades and in some cases perhaps even younger.…”

“…Three stars in our list of the PB stars have spectroscopic temperatures determined recently by Gonzalez et al (2001); these temperatures turned out to coincide with our uvby-based values within ∼50 K. One more star, t Boo, has the uvby temperature the same-within uncertainties-as in Fuhrman et al (1998) and the most recent estimate from spectroscopy in Gonzalez & Laws (2000).…”

Chromospheric activities and kinematics for solar type dwarfs and subgiants: analysis of the activity distribution and the AVR

“…If this is the case, and since we know planet formation is an integral part of the star formation and early stellar evolution process, then it stands to reason that dynamical formation of planets will affect their host stars to some degree. An example of this is the current model proposed by Bouvier (2008) to explain the observed depletion of lithium in planet-host stars (Gonzalez & Laws 2000;Israelian et al 2009). Therefore, it could be that stars with ages below ∼1 Gyr are accreting planets/planetesimals, transferring some angular momentum onto the host star and once the system is dynamically stable the star is free to rotationally stabilise and follow the evolution of the other two scenarios mentioned above.…”

Statistical cataloging of archival data for luminosity class IV–V stars

“…They apply to the values of θ from the sources cited in the first column. d Contributing papers are Gonzalez (1998), Gonzalez & Vanture (1998), Gonzalez et al (1999), Gonzalez & Laws (2000), and Gonzalez et al (2001). e The entries to the right apply if θ S ≤ 0.885.…”