  We examine 3 analytic theories of magnetospheric accretion onto classical T
Tauri stars under the assumption that the magnetic field strength does not vary
appreciably from star to star. From these investigations we derive predicted
relationships among the stellar mass, radius, rotation period, and disk
accretion rate. Data from 5 studies of the accretion parameters of CTTSs are
used to test the predicted correlations. We generally find that the data do not
display the predicted correlations except for that predicted by the model of
Shu et al. as detailed by Ostriker and Shu and extended here to include
non-dipole field topologies. Their identification of the trapped flux as an
important quantity in the model appears to be critical for reconciling the
observed data to the theory. While the data do generally support the extended
Ostriker and Shu predictions, only one of the two studies for which the
requisite data exist show the highest correlation when considering all the
relevant parameters. This suggests great care must be taken when trying to use
existing observations to test the theory.
