Abstract

This paper will primarily focus on a study by \cite{Shiode_2013} on how gravity modes could be excited by convection in massive main sequence stars. The first portion of this paper will explain the more commonly understood method of how gravity modes are driven by adiabatic expansion at the core and why gravity modes produced this way are so difficult to observe. The second part of this paper will briefly go over the methods for detecting gravity modes and the observational challenges faced. The third portion will look at models \cite{Shiode_2013} constructed using the MESA stellar evolution code that were used to estimate mode frequencies, excitation amplitudes and where in the stellar interior of various sized main sequence stars, gravity modes would propagate. The final portion of this paper will look at future advancements in detecting gravity modes and promising observations taken from the Kepler space satellite.