Oscillations in the G-type Giants

TL;DR

This study presents precise radial-velocity measurements of four G-type giants, revealing oscillation modes, frequency patterns, and damping times consistent with theoretical predictions, enhancing understanding of stellar oscillations in evolved stars.

Contribution

The paper provides detailed observational evidence of oscillation modes, including non-radial modes, in G-type giants, confirming theoretical models and scaling laws for stellar oscillations.

Findings

Detected short-term oscillations with amplitudes 1-7 m/s and periods 3-10 hours.

Confirmed that peak frequencies and large separations agree with scaling law predictions.

Identified non-radial modes through echelle diagrams, supporting theoretical mode predictions.

Abstract

The precise radial-velocity measurements of 4 G-type giants, 11Com, $\zeta$ Hya, $\epsilon$ Tau, and $\eta$ Her were carried out. The short-term variations with amplitudes, 1-7m/s and periods, 3-10 hours were detected. A period analysis shows that the individual power distribution is in a Gaussian shape and their peak frequencies ($\nu_{max}$) are in a good agreement with the prediction by the scaling law. With using a pre-whitening procedure, significant frequency peaks more than 3 $\sigma$ are extracted for these giants. From these peaks, we determined the large frequency separation by constructing highest peak distribution of collapsed power spectrum, which is also in good agreement with what the scaling law for the large separation predicts. Echelle diagrams of oscillation frequency were created based on the extracted large separations, which is very useful to clarify the properties of oscillation modes. In these echelle diagrams, odd-even mode sequences are clearly seen. Therefore, it is certain that in these G-type giants, non-radial modes are detected in addition to radial mode. As a consequence, these properties of oscillation modes are shown to follow what Dzymbowski et al.(2001) and Dupret et al.(2009) theoretically predicted. Damping times for these giants were estimated with the same method as that developed by Stello et al.(2004). The relation of Q value (ratio of damping time to period) to the period was discussed by adding the data of the other stars ranging from dwarfs to giants.