prototype of a class of variable stars called eclipsing binaries (eclipsing variable star), the second brightest star in the northern constellation Perseus. Its apparent visual magnitude changes over the range of (approximately) 2.2 to 3.5 with a period of 2.87 days. Even at its dimmest it remains readily visible to the unaided eye. The name probably derives from an Arabic phrase meaning “demon,” or “mischief-maker,” and the Arabs may have been aware of the star's variability even before the invention of the telescope.

The first European astronomer to note the light variation was the Italian Geminiano Montanari in 1670; the English astronomer John Goodricke (Goodricke, John) measured the cycle (69 hours) in 1782 and suggested partial eclipses of the star by another body as a cause, a hypothesis proved correct in 1889. The comparatively long duration of the eclipse shows that the dimensions of the two stars are not negligible in comparison with the distance between them. A third star, which does not take part in the eclipses, revolves about the other two with a period of 1.862 years.