We interpret the radio/X-ray correlation of LR ∝ LX~1.4 for LX/LEdd ≳ 10−3 with a detailed disk corona-jet model, in which the accretion flow and the jet are connected by a parameter, η, describing the fraction of the matter in the accretion flow ejected outward to form the jet. We calculate LR and LX at different Ṁ, adjusting η to fit the observed radio/X-ray correlation of the black hole X-ray transient H1743-322 for LX/LEdd > 10−3. It is found that the value of η for this radio/X-ray correlation for LX/LEdd > 10−3, is systematically less than that of the case for LX/LEdd < 10−3, which is consistent with the general idea that the jet is often relatively suppressed at the high luminosity phase in black hole X-ray binaries.