Asteroseismology of the Transiting Exoplanet Host HD 17156 with HST FGS

TL;DR

This study used HST FGS observations to detect stellar oscillations in HD 17156, enabling precise determination of its density, mass, radius, and age, marking a pioneering integration of asteroseismology with transiting exoplanet analysis.

Contribution

First direct stellar density measurement combining asteroseismology and transiting planet data, improving stellar parameter accuracy.

Findings

Detected p-modes in HD 17156 with high precision.

Derived stellar density of 0.5301 g/cm^3.

Estimated stellar mass, radius, and age with high accuracy.

Abstract

Observations conducted with the Fine Guidance Sensor on Hubble Space Telescope (HST) providing high cadence and precision time-series photometry were obtained over 10 consecutive days in December 2008 on the host star of the transiting exoplanet HD 17156b. During this time 10^12 photons (corrected for detector deadtime) were collected in which a noise level of 163 parts per million per 30 second sum resulted, thus providing excellent sensitivity to detection of the analog of the solar 5-minute p-mode oscillations. For HD 17156 robust detection of p-modes supports determination of the stellar mean density of 0.5301 +/- 0.0044 g/cm^3 from a detailed fit to the observed frequencies of modes of degree l = 0, 1, and 2. This is the first star for which direct determination of the mean stellar density has been possible using both asteroseismology and detailed analysis of a transiting planet light curve. Using the density constraint from asteroseismology, and stellar evolution modeling results in M_star = 1.285 +/- 0.026 solar, R_star = 1.507 +/- 0.012 solar, and a stellar age of 3.2 +/- 0.3 Gyr.