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The photospheric magnetic field outside of active regions and the network hasa ubiquitous and dynamic line-of-sight component that strengthens from diskcenter to limb as expected for a nearly horizontal orientation. This componentshows a striking time variation with an average temporal rms near the limb of1.7 G at ~3" resolution. In our moderate resolution observations the nearlyhorizontal component has a frequency variation power law exponent of -1.4 below1.5 mHz and is spatially patchy on scales up to ~15 arcsec. The field may be amanifestation of changing magnetic connections between eruptions and evolutionof small magnetic flux elements in response to convective motions. It shows nodetectable latitude or longitude variations.Comment: 7 pages, 6 figures, submitted to ApJ letters, quality of figures  significantly degraded here by compression requirement

Seething Horizontal Magnetic Fields in the Quiet Solar Photosphere