A hopeful prospect for the detection of g-modes is through gravitational wave detection. The ESA/NASA mission LISA could potentially have lowered the upper limit by a few mm/s in only a year of observing time\cite{Appourchaux_2003}. LISA would have been a gravitational wave telescope and would have been able to detect gravity waves coming from the oscillations deep within the sun’s interior. However, the mission was canceled due to lack of funding, but a similar mission by the ESA called ASTROD may still be underway. It would operate with two spacecrafts located on the far side of the sun in Earth’s orbit and use similar equipment to that of mission LISA to detect gravitational waves. This would dramatically lower the upper amplitude detection limit.

Recent analysis of Kepler satellite data by \cite{Balona_2011} have shown low frequency modes in slowly pulsating B-type(SPB) stars. \cite{Balona_2011} claims that seven stars in their study show evidence of g-modes. Figure 4 shows one of those seven, KIC 10960750. The figure shows the majority of frequencies below 3 \({d}^{-1}\) which are in the accepted range of for a g mode. Even though the majority of the detected amplitudes do not exceed 700 ppm, the Kepler data used was taken over 320 days, which allowed much of the noise to be factored out. The current noise level is only several ppm \cite{Balona_2011}. These distinct modes being primarily low frequency fit well with the convective excitation spectrum discussed in section 4.2. This demonstrates strong evidence for an observationally detected g mode. \cite{Balona_2011} also claims that some of the higher frequency modes, like the one at 10.449 \({d}^{-1}\) for KIC 10960750 in Figure 4, may actually be g modes themselves and that the star’s rotational frequency may be leading to scattering low frequency modes into frequencies that appear higher to the observer \cite{Balona_2011}.