Flux rope merging and the structure of switchbacks in the solar wind

TL;DR

This paper investigates how magnetic flux rope merging influences the structure of switchbacks in the solar wind, combining observations, analysis, and simulations to explain their formation, evolution, and magnetic characteristics.

Contribution

It introduces a flux rope merging model that explains the magnetic and structural features of switchbacks, supported by analytic, observational, and numerical evidence.

Findings

Flux rope merging reduces magnetic wrapping and elongation of switchbacks.

Dominance of axial magnetic field causes sharp magnetic rotations at switchback boundaries.

Switchback area scaling suggests observational probability is independent of heliocentric distance.

Abstract

A major discovery of Parker Solar Probe (PSP) was the presence of large numbers of localized increases in the radial solar wind speed and associated sharp deflections of the magnetic field - switchbacks (SB). A possible generation mechanism of SBs is through magnetic reconnection between open and closed magnetic flux near the solar surface, termed interchange reconnection that leads to the ejection of flux ropes (FR) into the solar wind. Observations also suggest that SBs undergo merging, consistent with a FR picture of these structures. The role of FRs merging in controlling the structure of SB in the solar wind is explored through direct observations, through analytic analysis, and numerical simulations. Analytic analysis reveals key features of the structure of FR and their scaling with the heliocentric distance R that are consistent with observations and that reveal the critical role of merging in controlling the SB structure. FR merging is shown to be energetically favorable to reduce the strength of the wrapping magnetic field and drive the observed elongation of SBs. A further consequence is the resulting dominance of the axial magnetic field within SBs that leads to the characteristic sharp rotation of the magnetic field into the axial direction at the SB boundary that is revealed in observations. Finally, the radial scaling of the SB area in the FR model of SBs suggests that the observational probability of SB identification should be insensitive to R, which is consistent with the most recent statistical analysis of SB observations from PSP.