Predicting the detectability of oscillations in solar-type stars observed by Kepler

TL;DR

This paper presents a method to estimate the likelihood of detecting solar-like oscillations in Kepler stars using basic stellar parameters, aiding asteroseismology in exoplanet research.

Contribution

It introduces a straightforward approach to predict oscillation detectability in Kepler targets based on temperature, radius, and magnitude, enhancing target selection for asteroseismic studies.

Findings

Provides a practical estimate method for oscillation detection.

Helps optimize Kepler target selection for asteroseismology.

Supports better constraints on exoplanetary system properties.

Abstract

Asteroseismology of solar-type stars has an important part to play in the exoplanet program of the NASA Kepler Mission. Precise and accurate inferences on the stellar properties that are made possible by the seismic data allow very tight constraints to be placed on the exoplanetary systems. Here, we outline how to make an estimate of the detectability of solar-like oscillations in any given Kepler target, using rough estimates of the temperature and radius, and the Kepler apparent magnitude.