Magnetic Reconnection of Solar Flux Tubes and Coronal Reconnection Signatures in the Solar Wind at 1 AU

The origin of interplanetary magnetic field that is frozen-in to the solar wind plasma flow is clearly magnetic flux from the Sun's corona. However, the filamented structure of magnetic fields observed in the solar wind cannot be accounted for quite so simply. Given the 2 days or more for solar wind to travel from the Sun to 1 AU, some argue that many current sheets are present due to turbulence and other in-transit effects in the dynamic plasma outflow. Alternatively, it is postulated that a "flux tube texture" of the solar wind exists as fossil structure of the corona. In this paper we examine the possible influence of magnetic reconnection occurring close to the Sun or in the solar wind on the character of current sheets observed by Magnetospheric Multiscale at 1 AU. Photospheric convection is used to perturb a magnetic carpet-like configuration, which has well-segmented open flux tubes defined by topological elements of the magnetic field. Flux tube boundaries in the model are defined by magnetic sepratrix surfaces which are a preferential location for strong currents and magnetic reconnection. Reconnection is associated with signatures in the magnetic field and plasma that may advect with the solar wind all the way to 1 AU. Aided by three-dimensional coronal modeling and two-dimensional simulation examples of reconnection layers, we examine properties of current sheets observed by Magnetospheric Multiscale and how these solar wind boundaries may relate to reconnection operating earlier in the solar wind or corona.