  We firstly present the Solar Dynamics Observatory observations of four
homologous flux ropes in active region (AR) 11745 on 2013 May 20-22. The four
flux ropes are all above the neutral line of the AR, with endpoints anchoring
at the same region, and have the generally similar morphology. For the first
three flux ropes, they rose up with a velocity of less than 30 km s$^{-1}$
after their appearances, and subsequently their intensities at 131 {\AA}
decreased and the flux ropes became obscure. The fourth flux rope erupted
ultimately with a speed of about 130 km s$^{-1}$ and formed a coronal mass
ejection. The associated filament showed an obvious anti-clockwise twist motion
at the initial stage, and the twist was estimated at 4$\pi$. This indicates
that kink instability possibly triggers the early rise of the fourth flux rope.
The activated filament material was spatially within the flux rope and they
showed consistent evolution in their early stages. Our findings provide new
clues for understanding the characteristics of flux ropes. Firstly, there are
multiple flux ropes that are successively formed at the same location during an
AR evolution process. Secondly, a slow-rise flux rope does not necessarily
result in a CME, and a fast-eruption flux rope results in a CME.
