TY - JOUR
T1 - Asteroseismology of the transiting exoplanet host HD 17156 with Hubble Space Telescope Fine Guidance Sensor
AU - Gilliland, Ronald L.
AU - McCullough, Peter R.
AU - Nelan, Edmund P.
AU - Brown, Timothy M.
AU - Charbonneau, David
AU - Nutzman, Philip
AU - Christensen-Dalsgaard, Jørgen
AU - Kjeldsen, Hans
PY - 2011/1/1
Y1 - 2011/1/1
N2 - Observations conducted with the Fine Guidance Sensor on the Hubble Space Telescope (HST) providing high cadence and precision time-series photometry were obtained over 10 consecutive days in 2008 December on the host star of the transiting exoplanet HD 17156b. During this time, 1.0 × 1012 photons (corrected for detector dead time) were collected in which a noise level of 163 parts per million per 30 s sum resulted, thus providing excellent sensitivity to the detection of the analog of the solar 5-minutep-mode oscillations. For HD 17156, robust detection of p modes supports the determination of the stellar mean density of (ρ*) = 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 the direct determination of (ρ*) 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* = 1.285 ± 0.026 M ⊙, R* = 1.507 ± 0.012 R ⊙, and a stellar age of 3.2 ± 0.3 Gyr.
AB - Observations conducted with the Fine Guidance Sensor on the Hubble Space Telescope (HST) providing high cadence and precision time-series photometry were obtained over 10 consecutive days in 2008 December on the host star of the transiting exoplanet HD 17156b. During this time, 1.0 × 1012 photons (corrected for detector dead time) were collected in which a noise level of 163 parts per million per 30 s sum resulted, thus providing excellent sensitivity to the detection of the analog of the solar 5-minutep-mode oscillations. For HD 17156, robust detection of p modes supports the determination of the stellar mean density of (ρ*) = 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 the direct determination of (ρ*) 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* = 1.285 ± 0.026 M ⊙, R* = 1.507 ± 0.012 R ⊙, and a stellar age of 3.2 ± 0.3 Gyr.
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U2 - 10.1088/0004-637X/726/1/2
DO - 10.1088/0004-637X/726/1/2
M3 - Article
AN - SCOPUS:84891213868
SN - 0004-637X
VL - 726
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
ER -