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We investigate the emergence of magnetic flux in the quiet Sun at very smallspatial scales, focusing on the magnetic connection between the photosphere andchromosphere. The observational data consist of spectropolarimetricmeasurements and filtergrams taken with the Hinode satellite and the Dutch OpenTelescope. We find that a significant fraction of the magnetic flux present ininternetwork regions appears in the form of Omega-shaped loops. The emergencerate is 0.02 loops per hour and arcsec^{-2}, which brings 1.1 x 10^12 Mx s^{-1}arcsec^{-2} of new flux to the solar surface. Initially, the loops are observedas small patches of linear polarization above a granular cell. Shortlyafterwards, two footpoints of opposite polarity become visible in circularpolarization within or at the edges of the granule and start to move toward theadjacent intergranular space. The orientation of the footpoints does not seemto obey Hale's polarity rules. The loops are continuously buffeted byconvective motions, but they always retain a high degree of coherence.Interestingly, 23% of the loops that emerge in the photosphere reach thechromosphere (16 cases out of 69). They are first detected in Fe I 630 nmmagnetograms and 5 minutes later in Mg I b 517.3 nm magnetograms. After about 8minutes, some of them are also observed in Ca II H line-core images, where thefootpoints produce small brightness enhancements.

Emergence of small-scale magnetic loops through the quiet solar atmosphere