Abstract
Both V409 Hya and GSC 2537-0520 are extreme mass-ratio binaries thought to arise from billions of years of evolution. During their history, the systems began as detached binaries and have gone through semidetached and contact stages and finally an "over contact configuration" due to long ages of magnetic breaking as experienced by solar type stars and binaries. This causes a steady but slow loss of angular momentum in the binary system and its subsequent coalescence. Contact and magnetic breaking results in the slow absorption of the smaller companion by the larger star and an extreme mass ratio smaller than 0.2. Eventually the system becomes unstable, leading to the formation of a single, fast-rotating subgiant FK Comaetype star. This is the leading explanation of the "blue straggler" population in star clusters. Long contact of the two stars causes the stars to equalize in temperature, and the large star becomes the main source of energy. This configuration means that the eclipses have equal depths. However, in our study of eclipsing binaries, we have discovered two extreme mass-ratio binaries with EB-type light curves-that is, the eclipse depths are quite different, and the component temperatures differ by hundreds of Kelvins. The existence of such binaries calls into question the long-age interpretation of such systems. The two binaries and their creationary implications will be discussed.