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The origin of switchbacks in the solar wind is discussed in two classes oftheory that differ in the location of the source being either in the transitionregion near the Sun or in the solar wind, itself. The two classes of theorydiffer in their predictions of the switchback rate as a function of distancefrom the Sun. To test these theories, one-hour averages of Parker Solar Probedata were summed over orbits three through seven. It is found that:  1. The average switchback rate was independent of distance from the Sun. 2.The average switchback rate increased with solar wind speed. 3. The switchbacksize perpendicular to the flow increased as R, the distance from the Sun, whilethe radial size increased as R2, resulting in a large and increasing switchbackaspect ratio with distance from the Sun. 4. The switchback rotation angle didnot depend on either the solar wind speed or the distance from the Sun.  These results are consistent with switchback formation in the transitionregion because their increase of tangential size with radius compensates forthe radial falloff of their equatorial density to produce switchback rates thatare independent of distance from the Sun. This constant observed switchbackrate is inconsistent with an in situ source. Once formed, the switchback sizeand aspect ratio, but not the rotation angle, increased with radial distance toat least 100 solar radii. In addition, quiet intervals between switchbackpatches occurred at the lowest solar wind speeds.

On the origin of switchbacks observed in the solar wind