Speaker
Description
Magnetic helicity as a measure of correlation of the magnetic field and electric current plays an important role in astrophysical 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 the solar turbulence, and therefore, observations of magnetic structures such as active regions may bring essential information on its global distribution and intrinsic evolution. Secondly, the local distribution and dynamics of its observational proxies is linked with the potential for solar flaring activity that may abruptly change the helicity balances.
We also review the observations that shed light on the spatial and temporal behavior of magnetic helicity in the Sun. The magnetic helicity being 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 dynamic behaviour of solar activity.
We show that important observable properties of the solar cycle can be obtained even with simple self-consistent models of solar dynamo with helicity. That enables us to understand dynamics of the solar cycle on relatively short and long ranges. That can also be used to envisage the dynamics of flaring activity.
The project is supported by Russian Science Foundation grant 21-72-20067
| Submit to 'solar physics' topical issue? | Maybe |
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