Eclipsing binary stars are stellar systems consisting of two or more stars where the orbital plane of the components align with the line of sight of an observer; this alignment can result in eclipses. These eclipses are seen as a characteristic dimming in the system's brightness when seen from Earth. The subclass β Persei-Type (Algol) binary, or EA type, are known as detached binaries. EA types are characterized by distinct eclipses in their phased light curves, i.e., it is easy to see when the eclipse begins and ends. Additionally, one should expect to see an almost constant magnitude before and after the eclipse. It is also common for these systems to have a small or insignificant secondary minimum. EA binaries span a large range of periods, from 0.2 days to many years!