Stellar Model Analysis of the Oscillation Spectrum of eta Bootis Obtained from MOST

Abstract

Eight consecutive low-frequency radial p-modes are identified in the G0 IV star eta Bootis based on 27 days of ultraprecise rapid photometry obtained by the MOST (Microvariability & Oscillations of Stars) satellite. The MOST data extend smoothly to lower overtones the sequence of radial p-modes reported in earlier groundbased spectroscopy by other groups. The lower-overtone modes from the MOST data constrain the interior structure of the model of eta Boo. With the interior fit anchored by the lower-overtone modes seen by MOST, standard models are not able to fit the higher-overtone modes with the same level of accuracy. The discrepancy is similar to the discrepancy that exists between the Sun's observed p-mode frequencies and the p-mode frequencies of the standard solar model. This discrepancy promises to be a powerful constraint on models of 3D convection.

arXiv comment30 pages with 14 figures. Accepted for publication in ApJ

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• 3D convection simulations of the outer layers of the Sun using realistic physics
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• Solar-like oscillations in the metal-poor subgiant nu Indi: constraining the mass and age using asteroseismology
• MADE: A spectroscopic Mass, Age, and Distance Estimator for red giant stars with Bayesian machine learning
• Nonradial p-modes in the G9.5 giant epsilon Oph? Pulsation model fits to MOST photometry
• Benchmark ages for the Gaia benchmark stars
• Reduction of time-resolved space-based CCD photometry developed for MOST Fabry Imaging data
• The nature of p-modes and granulation in HD 49933 observed by CoRoT
• The Current Status of Asteroseismology
• Measurement of the Surface Gravity of $\eta$ Boo
• Space and Ground Based Pulsation Data of Eta Bootis Explained with Stellar Models Including Turbulence