  We present a method that uses disk models to determine stellar masses for
Pre-Main sequence T Tauri stars from JHK photometry. We find that the infrared
excess produced by the disk behaves in a similar way to the extinction vector
when plotted on color-color and color-magnitude diagrams, but that it is
linearly independent. Employing these vectors as a basis of a vector space we
carry out a coordinate transformation that allows us to find the mass of a
central star for a given age. To test this Principal Vectors (PV) method we
compare the mass values (MPV) obtained for 14 T Tauri objects in the
Taurus-Auriga region with mass values known by dynamical methods. Further on,
we analyzed 4 systems with multiple components (GG Tau, FO Tau, FS Tau, and
V733 Tau) and determined the mass for each component of the system. We analyzed
the effect of using different evolutionary models and other parameter values.
