  We make predictions of the detectability of low-frequency p modes. Estimates
of the powers and damping times of these low-frequency modes are found by
extrapolating the observed powers and widths of higher-frequency modes with
large observed signal-to-noise ratios. The extrapolations predict that the
low-frequency modes will have small signal-to-noise ratios and narrow widths in
a frequency-power spectrum. Monte Carlo simulations were then performed where
timeseries containing mode signals and normally distributed Gaussian noise were
produced. The mode signals were simulated to have the powers and damping times
predicted by the extrapolations. Various statistical tests were then performed
on the frequency-amplitude spectra formed from these timeseries to investigate
the fraction of spectra in which the modes could be detected. The results of
these simulations were then compared to the number of p-modes candidates
observed in real Sun-as-a-star data at low frequencies. The fraction of
simulated spectra in which modes were detected decreases rapidly as the
frequency of modes decreases and so the fraction of simulations in which the
low-frequency modes were detected was very small. However, increasing the
signal-to-noise (S/N) ratio of the low-frequency modes by a factor of 2 above
the extrapolated values led to significantly more detections. Therefore efforts
should continue to further improve the quality of solar data that is currently
available.
