Authors: Mariana Jeunon (NASA GSFC/CUA), Sanchita Pal (NASA GSFC/GMU), Fernando Carcaboso (NASA GSFC), Teresa Nieves-Chinchilla (NASA GSFC), Georgia De Nolfo (NASA GSFC), Eric Christian (NASA GSFC), Andreas J Weiss (NASA GSFC)

Interplanetary Coronal Mass Ejections (ICMEs) entrain mass and magnetic energy from the Sun to the Heliosphere. A subset of these ICMEs are Magnetic Clouds (MCs), also known as Magnetic Flux Ropes (MFRs), are characterized by an enhanced magnetic field strength, a smooth rotation of the magnetic field vector, and a low proton temperature. These MRFs contain twisted flux tubes, which provide an organized magnetic structure entraining confined plasma. That way, the magnetic helicity coming from the Sun into the heliosphere is transported. As these ICMES travel through the interplanetary space, they can interact with the solar wind and suffer magnetic reconnection. This reconnection leads to a change in the internal structures of the MCs, a process we call erosion. By looking into the azimuthal magnetic flux and signatures of reconnection, we can further study the process of erosion. In this work, we will explore the effects of such erosion in the magnetic field configuration of the heliospheric flux ropes.