  Low frequency dynamic spectra of radio bursts from nearby stars offer the
best chance to directly detect the stellar signature of transient mass loss on
low mass stars. Crosley et al. (2016) proposes a multi-wavelength methodology
to determine coronal mass ejection parameters, such as Coronal Mass Ejection
(CME) speed, mass, and kinetic energy.
  We test the validity and accuracy of the results derived from the methodology
by using Geostationary Operational Environmental Satellite X-ray observations
and Bruny Island Radio Spectrometer radio observations. These are analogous
observations to those which would be found in the stellar studies. Derived
results from these observations are compared to direct white light measurements
of the Large Angle and Spectrometric Coronagraph.
  We find that, when a pre-event temperature can be determined, that the
accuracy of CME speeds are within a few hundred km/s, and are reliable when
specific criteria has been met. CME mass and kinetic energies are only useful
in determining approximate order of magnitude measurements when considering the
large errors associated to them. These results will be directly applicable to
interpretation of any detected stellar events and derivation of stellar CME
properties.
