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Small-scale internetwork (IN) features are thought to be the major source offresh magnetic flux in the quiet Sun. During its first science flight in 2009,the balloon-borne observatory Sunrise captured images of the magnetic fields inthe quiet Sun at a high spatial resolution. Using these data we measure therate at which the IN features bring magnetic flux to the solar surface. In aprevious paper it was found that the lowest magnetic flux in small-scalefeatures detected using the Sunrise observations is 9 x 10^14 Mx. This isnearly an order of magnitude smaller than the smallest fluxes of featuresdetected in observations from the Hinode satellite. In this paper, we computethe flux emergence rate (FER) by accounting for such small fluxes, which wasnot possible before Sunrise. By tracking the features with fluxes in the range10^15-10^18 Mx, we measure an FER of 1100 Mx cm^-2 day^-1. The smaller featureswith fluxes less than or equal to 10^16 Mx are found to be the dominantcontributors to the solar magnetic flux. The FER found here is an order ofmagnitude higher than the rate from Hinode, obtained with a similar featuretracking technique. A wider comparison with the literature shows, however, thatthe exact technique of determining the rate of the appearance of new flux canlead to results that differ by up to two orders of magnitude, even when appliedto similar data. The causes of this discrepancy are discussed and firstqualitative explanations proposed.

Estimation of the magnetic flux emergence rate in the quiet Sun from Sunrise data