Redistribution of magnetic helicity at the Sun

Evolution of magnetic loops associated with filaments and coronal mass ejections involves a redistribution of solar magnetic helicity. Two mechanisms of the helicity redistribution are discussed. The first one involves magnetic reconnections among magnetic loops and can introduce helicity into an erupting magnetic field accompanied with an encapture of helicity by the Sun. The second one involves the MHD helicity redistribution in the Sun and indicates that the magnetic helicity of each hemisphere of the Sun oscillates about a mean with the half‐period of the solar cycle (11 years), but does not change sign from one 11 year period to the next.