To be an eclipsing binary, the binary is seen nearly edge-on (i.e., at an inclination relative to the line of sight of nearly 90°).
If only one component star's spectral lines are seen the binary is a single-lined spectroscopic binary.
If spectral lines are seen from both component stars, the binary is a double-lined spectroscopic binary.
Visual binaries are those that can be resolved into two stars.
There may be some eclipsing binaries that are visual binaries, but yours truly knows of none.
All one can determine for a double-lined spectroscopic binary is the quantity m*sin(i)**3, where m is the stellar mass of a component star, i is inclination, and sin is the sine function. We know even less about the stellar mass of single-lined spectroscopic binaries (e.g., Shane Larson: Binary Stars).
However, for an eclipsing binary, we know inclination i ≅ 90°. So at least for double-lined spectroscopic binaries we can determine the component stellar masses to some accuracy.
One can, of course, determine mass for stars by modeling and stellar spectroscopic data, but those results are then model-dependent, of course.
The other method is the Doppler spectroscopy method.