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We compare the magnetic helicity in the 17-18 March 2013 interplanetarycoronal mass ejection (ICME) flux-rope at 1 AU and in its solar counterpart.The progenitor coronal mass ejection (CME) erupted on 15 March 2013 from NOAAactive region 11692 and associated with an M1.1 flare. We derive the sourceregion reconnection flux using post-eruption arcade (PEA) method (Gopalswamy etal. 2017a) that uses the photospheric magnetogram and the area under the PEA.The geometrical properties of the near-Sun flux rope is obtained byforward-modeling of white-light CME observations. Combining the geometricalproperties and the reconnection flux we extract the magnetic properties of theCME flux rope (Gopalswamy et al. 2017b). We derive the magnetic helicity of theflux rope using its magnetic and geometric properties obtained near the Sun andat 1 AU. We use a constant-{\alpha} force-free cylindrical flux rope model fitto the in situ observations in order to derive the magnetic and geometricinformation of the 1-AU ICME. We find a good correspondence in both amplitudeand sign of the helicity between the ICME and the CME assuming a semi-circular(half torus) ICME flux rope with a length of {\pi} AU. We find that about 83%of the total flux rope helicity at 1 AU is injected by the magneticreconnection in the low corona. We discuss the effect of assuming flux ropelength in the derived value of the magnetic helicity. This study connecting thehelicity of magnetic flux ropes through the Sun-Earth system has importantimplications for the origin of helicity in the interplanetary medium and thetopology of ICME flux ropes at 1 AU and hence their space weather consequences.

A Sun-to-Earth analysis of magnetic helicity of the 17-18 March 2013 interplanetary coronal mass ejection