A homogeneous spectroscopic analysis of host stars of transiting planets

TL;DR

This study provides a homogeneous set of spectroscopic parameters for 13 transiting planet host stars, improving the accuracy of stellar and planetary property determinations and supporting the analysis of planet formation correlations.

Contribution

It offers uniformly derived stellar parameters for 13 transiting planet hosts, including effective temperature, gravity, and metallicity, with a comprehensive dataset of 50 objects for future research.

Findings

New parameters often differ from previous estimates, affecting planetary radius calculations.

Systematic offset in abundance scale for TrES and HAT objects.

Iron abundance distribution aligns with known metal-rich planet host stars.

Abstract

The analysis of transiting extra-solar planets provides an enormous amount of information about the formation and evolution of planetary systems. A precise knowledge of the host stars is necessary to derive the planetary properties accurately. The properties of the host stars, especially their chemical composition, are also of interest in their own right. Information about planet formation is inferred by, among others, correlations between different parameters such as the orbital period and the metallicity of the host stars. The stellar properties studied should be derived as homogeneously as possible. The present work provides new, uniformly derived parameters for 13 host stars of transiting planets. Effective temperature, surface gravity, microturbulence parameter, and iron abundance were derived from spectra of both high signal-to-noise ratio and high resolution by assuming iron excitation and ionization equilibria. For some stars, the new parameters differ from previous determinations, which is indicative of changes in the planetary radii. A systematic offset in the abundance scale with respect to previous assessments is found for the TrES and HAT objects. Our abundance measurements are remarkably robust in terms of the uncertainties in surface gravities. The iron abundances measured in the present work are supplemented by all previous determinations using the same analysis technique. The distribution of iron abundance then agrees well with the known metal-rich distribution of planet host stars. To facilitate future studies, the spectroscopic results of the current work are supplemented by the findings for other host stars of transiting planets, for a total dataset of 50 objects.