Helicity transport from the convection zone to interplanetary space

Zhang Mei, zhangmei@bao.ac.cn, National Astronomical Observatory

Abstract
Solar magnetic field, created by solar dynamo in the convection zone, is dissipated via processes such as solar flares, coronal mass ejections (CMEs) as well as solar winds. In this talk, I will focus on how magnetic helicity, created by solar dynamo, is dissipated (transported, more actually speaking) from the convection zone to the corona and then into the interplanetary space. Related topics include: what are the possible processes that produce the observed hemispheric helicity sign rule; why are magnetic flux ropes to be formed in the corona; what are the photospheric evidences of magnetic reconnection in the corona; why are CMEs the unavoidable products of coronal evolution; and in what forms would the interplanetary space accommodate the large amount of magnetic helicity that solar dynamo has been continuously producing.