  We observed the flare stars AD Leonis, Wolf 424, EQ Pegasi, EV Lacertae, and
UV Ceti for nearly 135 hours. These stars were observed between 63 and 83 MHz
using the interferometry mode of the Long Wavelength Array. Given that emission
from flare stars is typically circularly polarized, we used the condition that
any significant detection present in Stokes I must also be present in Stokes V
at the same time in order for us to consider it a possible flare. Following
this, we made one marginal flare detection for the star EQ Pegasi. This flare
had a flux density of 5.91 Jy in Stokes I and 5.13 Jy in Stokes V,
corresponding to a brightness temperature $1.75 \times 10^{16}(r/r_*)^{-2}$ K.
