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We study the structure of the photospheric magnetic field of the quiet Sun byinvestigating weak spectro-polarimetric signals. We took a sequence of Stokesspectra of the Fe I 630.15 nm and 630.25 nm lines in a region of quiet Sun nearthe disk center, using the POLIS spectro-polarimeter at the German VTT onTenerife. The line cores of these two lines form at different heights in theatmosphere. The 3$\sigma$ noise level of the data is about 1.8 $\times 10^{-3}I_{c}$. We present co-temporal and co-spatial Stokes-$V$ profiles of the Fe I630 nm line pair, where the two lines show opposite polarities in a singlespectrum. We compute synthetic line profiles and reproduce these spectra with atwo-component model atmosphere: a non-magnetic component and a magneticcomponent. The magnetic component consists of two magnetic layers with oppositepolarity: the upper one moves upwards while the lower one moves downward.In-between, there is a region of enhanced temperature. The Stokes-$V$ line pairof opposite polarity in a single spectrum can be understood as a magneticreconnection event in the solar photosphere. We demonstrate that such ascenario is realistic, but the solution may not be unique.

Opposite magnetic polarity of two photospheric lines in single spectrum of the quiet Sun