Astronomy and Astrophysics, volume 537A, 9-9 (2012/1-1)
Solar-like oscillations in the G9.5 subgiant β Aquilae.
CORSARO E., GRUNDAHL F., LECCIA S., BONANNO A., KJELDSEN H. and PATERNO L.
Abstract (from CDS):
An interesting asteroseismic target is the G9.5 IV solar-like star β Aql. This is an ideal target for asteroseismic investigations, because precise astrometric measurements are available from Hipparcos that greatly help in constraining the theoretical interpretation of the results. The star was observed during six nights in August 2009 by means of the high-resolution echelle spectrograph SARG operating with the TNG 3.58m Italian telescope (Telescopio Nazionale Galileo) on the Canary Islands, exploiting the iodine cell technique. We present the result and the detailed analysis of high-precision radial velocity measurements, where the possibility of detecting individual p-mode frequencies for the first time and deriving their corresponding asymptotic values will be discussed. The Fourier analysis technique based on radial velocity time series and the fitting of asymptotic relation to the power spectrum were the main tools used for the detection of the asteroseismic parameters of the star. The time-series analysis carried out from ∼800 collected spectra shows the typical p-mode frequency pattern with a maximum centered at 416µHz. In the frequency range 300-600µHz we identified for the first time six high signal-to-noise ratio (S/N>3.5) modes with l=0,2 and 11<n<16 and three possible candidates for mixed modes (l=1), although the p-mode identification for this type of star appears to be quite difficult owing to a substantial presence of avoided crossings. The large frequency separation and the surface term from the set of identified modes by means of the asymptotic relation were derived for the first time. Their values are Δν=29.56±0.10µHz and ε=1.29±0.04, consistent with expectations. The most likely value for the small separation is δν02=2.55±0.71µHz.