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Parker Solar Probe (PSP) has shown that the solar wind in the innerheliosphere is characterized by the quasi omni-presence of magnetic switchbacks("switchback" hereinafter), local backward-bends of magnetic field lines.Switchbacks also tend to come in patches, with a large-scale modulation thatappears to have a spatial scale size comparable to supergranulation on the Sun.Here we inspect data from the first ten encounters of PSP focusing on differenttime intervals when clear switchback patches were observed by PSP. We show thatthe switchbacks modulation, on a timescale of several hours, seems to beindependent of whether PSP is near perihelion, when it rapidly traverses largeswaths of longitude remaining at the same heliocentric distance, or near theradial-scan part of its orbit, when PSP hovers over the same longitude on theSun while rapidly moving radially inwards or outwards. This implies thatswitchback patches must also have an intrinsically temporal modulation mostprobably originating at the Sun. Between two consecutive patches, the magneticfield is usually very quiescent with weak fluctuations. We compare variousparameters between the quiescent intervals and the switchback intervals. Theresults show that the quiescent intervals are typically less Alfv\'enic thanswitchback intervals, and the magnetic power spectrum is usually shallower inquiescent intervals. We propose that the temporal modulation of switchbackpatches may be related to the "breathing" of emerging flux that appears inimages as the formation of "bubbles" below prominences in the Hinode/SOTobservations.

Patches of magnetic switchbacks and their origins