We have fit the normal , well observed , Type Ia Supernova ( SN Ia ) SN 1994D with non-LTE spectra of the deflagration model W7 .
We find that well before maximum luminosity W7 fits the optical spectra of SN 1994D .
After maximum brightness the quality of the fits weakens as the spectrum forms in a core rich in iron peak elements .
We show the basic structure of W7 is likely to be representative of the typical SN Ia .
We have shown that like W7 , the typical SN Ia has a layer of unburned C+O composition at v > 15000 km s ^ { -1 } , followed by layers of C-burned and O-burned material with a density structure similar to W7 .
We present UVOIR ( UBVRIJKH ) synthetic photometry and colors and compare with observation .
We have computed the distance to the host galaxy , NGC 4526 , obtaining a distance modulus of \mu = 30.8 \pm 0.3 .
We discuss further application of this direct measurement of SNe Ia distances .
We also discuss some simple modifications to W7 that could improve the quality of the fits to the observations .