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The field of asteroseismology has undergone a revolution in recent years largely due to the vast amounts of high-quality data coming from space missions such as \textit{Kepler}. This has uncovered the need for a better understanding of the near-surface layers of solar-type stars, where vigorous convection gives rise to granulation features on the stellar surface. In this manuscript I briefly review a few important concepts relating to asteroseismology of solar-like stars, after which I describe some research ideas related to combining asteroseismology and \co hydrodynamical simulations with a goal of learning more about the stellar granulation.

We present the first detections by the NASA K2 Mission of oscillations in solar-type stars, using short-cadence data collected during K2 Campaign\,1 (C1). We understand the asteroseismic detection thresholds for C1-like levels of photometric performance, and we can detect oscillations in subgiants having dominant oscillation frequencies around $1000\,\rm \mu Hz$. Changes to the operation of the fine-guidance sensors are expected to give significant improvements in the high-frequency performance from C3 onwards. A reduction in the excess high-frequency noise by a factor of two-and-a-half in amplitude would bring main-sequence stars with dominant oscillation frequencies as high as ${\simeq 2500}\,\rm \mu Hz$ into play as potential asteroseismic targets for K2., Comment: Accepted for publication in PASP; 16 pages, 2 figures