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One "strong" magnetic cloud (MC) with the magnetic field magnitude reaching$\sim$ 40 nT at 1 au during 2012 June 16-17 is examined in association with apre-existing magnetic flux rope (MFR) identified on the Sun. The MC ischaracterized by a quasi-three dimensional (3D) flux rope model based on insitu measurements from the Wind spacecraft. The magnetic flux contents andother parameters are quantified. In addition, a correlative study with thecorresponding measurements of the same structure crossed by the Venus Express(VEX) spacecraft at a heliocentric distance 0.7 au and with an angularseparation $\sim 6^\circ$ in longitude is performed to validate the MC modelingresults. The spatial variation between the Wind and VEX magnetic fieldmeasurements is attributed to the 3D configuration of the structure as featuredby a knotted bundle of flux. The comparison of the magnetic flux contentsbetween the MC and the source region on the Sun indicates that the 3Dreconnection process accompanying an M1.9 flare may correspond to the magneticreconnection between the field lines of the pre-existing MFR rooted in theopposite polarity footpoints. Such a process reduces the amount of the axialmagnetic flux in the erupted flux rope, by approximately 50\%, in this case.

Validation and interpretation of three-dimensional configuration of a magnetic cloud flux rope