Observational proxies of magnetic helicity in the Sun, its origin, transport, and role in the solar dynamo models
Dr Kirill Kuzanyan
Wednesday 16th November, 2022 15:00-16:00 Maths 110/ ZOOM (ID: 869 8618 2208)
Abstract
Magnetic helicity plays an important role in magnetohydrodynamics as an inviscid invariant. In the context of solar physics, it is extremely important in several aspects. Firstly, its relaxation time is much longer than the turnover time of solar turbulence, and therefore observations of magnetic structures such as active regions may bring essential information for knowledge of its global distribution. Secondly, the local distribution and dynamics of its observational proxies is linked with the potential for solar flaring activity. And more, the transport of magnetic helicity which is generated by the solar dynamo mechanism and released to the heliosphere (where it is taken out by the solar wind) provides an important constraint to the dynamo models. The balance of helicity plays a role of a nonlinear feedback which determines complexity of dynamics of the solar activity. We show that important observable properties of solar cyclicity can be obtained even with simple self-consistent models of solar dynamo with helicity.
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