The possibility of the binary origin for the central compact objects (CCOs) is probed in this paper. Firstly, we find that the CCOs share the similar average spin period to the normal supernova remnant (SNR) pulsars, however, the average surface magnetic field strength of CCOs (B  5.41010 Gs) is lower than the normal SNR pulsars (B  7.71012 Gs) by  2 orders of magnitudes. Meantime, we also find that almost all the normal SNR pulsars lie in the position above the spin-up line, while all the CCOs lie in the position under the spin-up line. Therefore, we doubt that CCOs may origin from the accretion induced spin-up process in the binaries. Secondly, we analyze the ossible binary evolution process of CCOs based on recycling theory of the neutron stars: in the binary, a CCO can accrete the ΔM  10?2M⊙ matter with the accretion rate of ˙M  1017 g
s?1 during the time of  106 yrs, then its spin period will decrease from P  10 s to P  0:1 s, and its surface magnetic field strength will decrease from B  1012 Gs to B  1010 Gs. Considering that the evolution timescale of  106 yr is far longer than the age of the SNRs containing CCOs ( 0:3–7 kyr), we suppose that CCOs may be the products of the supernova of the first star in the binary,and the binary is disintegrated during the supernova of the second star, which leaves a CCO and the SNR of the second star. This model predicts that there may exit a young normal pulsar near the CCO (P  0:02 s, B  1012 Gs), and we expect that the radio telescope and high energy detector can survey these sources in the future.