Formation of Unique Magnetic Structures Observed in the Inner Heliosphere: from Braids to Knots

Some of the unique features observed by Parker Solar Probe (PSP) spacecraft on its first incursions into the inner heliosphere consist of rapid polarity inversions of the mostly radial magnetic field embedded into the solar wind. These so-called switchbacks whose precise origin is still unknown, together with local enhancements in the radial plasma jet speed point out to coronal source of complex magnetic structures subsequently injected into the solar wind flow, with potentially significant effects on the dynamics of the magnetic field and the ensuing plasma activity. The switchbacks which were conjectured previously by Helios and Ulysses satellites mainly in the fast solar wind, together with their numerous PSP observations in the slow solar wind indicate a sustained stability of these configurations over wide range of heliocentric distances. We present here a comprehensive scenario connecting (a) remote high resolution solar observations of braided fields with predictions for future higher resolution coronal oscillations; (b) bi-modal reconnection resulting either in (i) disintegration of the braids resulting in coronal heating or in (ii) braid morphism into magnetic knot structures; (c) incorporation of these knotted magnetic structures into the solar wind while their stability controlled by intrinsic invariants and (d) intermittent recombination of knots into a train of inversions due to magnetic knot addition, resulting in structures seen by PSP traversing the switchbacks. All these processes are incorporated into topological aspects of braid and knot theory. Similar outcome, although at different scenario, may apply to outflows phenomena during planet formation and to laboratory experiments of high-energy density jets driven by toroidal magnetic field.