Uncovering the process that transports magnetic helicity to coronal mass ejection flux ropes

Magnetic helicity, an intrinsic property of eruptive helical flux ropes (FRs) forming coronal mass ejections (CMEs), plays important role in determining CME geoeffectiveness. In the solar atmosphere and heliosphere, helicity remains conserved a closed volume. Considering this fact as basis our study, we perform quantitative comparison between total magnetic twisted interplanetary CMEs those transported to via reconnection at low corona. At source, twisted/poloidal ( ? pcme ) is directly estimated from flux, H cme obtained by combining information with physical parameters. 1 AU, pmc mc are situ observations. uncertainties steaming FR length, parameter estimations, poloidal AU found be highly relevant = 0.4–1.5, 0.3–1) low-corona wake CMEs. This result unchanged despite association pre-existing FRs. We show that significant reduction during its heliospheric propagation may high rate erosion medium. Our event analysis confirms CME’s properties FRs sheared arcades. A one-to-one correspondence chirality 1-AU their pre-eruptive structures complies sense field line rotations remain source. By connecting through Sun-Earth medium, study provides implications for origin geoeffectiveness