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Exploring Current and Magnetic Helicity in Solar Physics: Insights from Higher Invariants

Discover the significance of current and magnetic helicity in solar physics, examining higher invariants post-helicity events. Delve into the complexities of magnetic field dynamics and explore the implications of linkages and mirror symmetry. Unravel the enigma of helicity patterns and understand the challenges in defining density. Explore the potential of polynomial invariants in analyzing helicity phenomena, and consider the implications for dynamo theories. Gain insights into helicity butterfly diagrams and mutual helicity relationships, paving the way for further research in solar physics.

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Exploring Current and Magnetic Helicity in Solar Physics: Insights from Higher Invariants

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  1. D.Sokoloff,Egor Illarionov Moscow State University, Russia Alexander Smirnov, Peter Akhmetyev IZMIRAN, Helicity Thinkshop on Solar Physics October 27-31, 2013, Beijing, China After current helicity: higher topological invariants

  2. What happens after an intensive time if new perspectives remain unclear (E.Much, Tag danach)

  3. Bufferfly diagramm for current helicity as observed at Huairou

  4. Why helicity data are instructive? • Current helicity – observable, clear topological meaning – linkage of current Mirror asymmetric • Magnetic helicity – topological invariant – linkage of magnetic lines Reconnections are slow – inviscid invariant of motion Can be in principle obtained from observations

  5. Difficulties • Magnetic tube is a not very elaborated concept. Magnetic line covers often a 3D domain. • How to resolve: Arnold suggested a technique of short ways. • We do not know magnetic field inside vthe Sun (and in some other domains as well). • How to resolve: relative helicity. Linkages in respect to a given field.

  6. How to use? • Magnetic field relaxation – is cxontrolled by magnetic helicty • Dynamo: dynamo generated mean field is helical. One have to conserve total helecity. • IMPORTANT: Magnetic helicity can not be transported along the spectrum: ab \sim aa/k >> vv for small k. Upper bound for helicity (no helicity without energy). Capacity of higher Levels is insufficient

  7. Magnetic helicity densityis gauge non-invariantHow to resolve: A natural gaugefollows from the local homogeneity and isotropy and axial symmetryOne can calculate magnetic helicity from the current one

  8. Magnetic helicity: algebraic sum of linkagesA cancellation of linkages can happen. Many other invariants are possible – say, sum of squares of linkages. Never vanishes if the field is linked. Polynomial invariants.

  9. Every two lines are non-linked, however 3 are linked.

  10. Let us deal for the time being with polynomial invariants only.A problem: density of the invariant+ of course, all other problems

  11. It remains unclear how to define the density

  12. Helicity patterns are similar in general to the sunspots pattern! Theory predicts a wrong time lag Unexpected areas of the «wrong» helicity sign Helicity butterfly diagrams: predicted, expected and observed. Very noisy as expected.Two observed diagrams are very similar! - effective suppression of the noise. .

  13. Mutual helicity c a

  14. Helicity invariants

  15. Conclusions:1. Higher (polynomial) invariants are in principle measurable from available data.2. This very invariant is mirror-symmetric (not very interesting for dynamo).To be clarified:1.Can these invariants be transported along the spectrum?2. What about other invariants?

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