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Switchbacks (rotations of the magnetic field) are observed on the ParkerSolar Probe. Their evolution, content, and plasma effects are studied in thispaper. The solar wind does not receive a net acceleration from switchbacks thatit encountered upstream of the observation point. The typical switchbackrotation angle increased with radial distance. Significant Poynting fluxesexisted inside, but not outside, switchbacks and they are related to theincreased EXB/B2 flow caused by the magnetic field rotating to become moreperpendicular to the flow direction. (Outside the switchbacks, the magneticfield and solar wind flow were generally radial.) The solar wind flow insideswitchbacks was faster than that outside due to the frozen-in ions moving withthe magnetic structure at the Alfven speed. This energy gain results from thedivergence of the Poynting flux from outside to inside the switchback, whichproduces a loss of electromagnetic energy on switchback entry and recovery ofthat energy on exit, with the lost energy appearing in the plasma flow.Switchbacks contain 0.3-10 Hz waves that may result from currents and theKelvin-Helmholtz instability that occurs at the switchback boundaries. Thesewaves may combine with lower frequency MHD waves to heat the plasma. The radialdecreases of the Poynting flux and solar wind speed inside switchbacks are dueto a geometrical effect.

Switchbacks in the solar magnetic field: their evolution, their content, and their effects on the plasma, V2