  We examine the hypothesis that multipolar magnetic fields advected by
photospheric granules can contribute heating to the active chromosphere and
corona. On 28 September 2020 the GRIS and HiFI+ instruments at the GREGOR
telescope obtained data of NOAA 12773. We analyze Stokes profiles of spectral
lines of Si I and He I, to study magnetic fields from photosphere to the upper
chromosphere. Magnetogram and EUV data from the HMI and AIA instruments on the
SDO spacecraft are co-aligned and studied in relation to the GRIS data. At
coronal loop footpoints, minor polarity fields comprise just 0.2% and 0.02% of
the flux measured over the 40" x 60" area observed in the photosphere and upper
chromosphere, centered 320" from disk center. Significantly, the minority
fields are situated >~ 12" from bright footpoints. We use physical arguments to
show that any unresolved minority flux cannot reach coronal footpoints adjacent
to the upper chromosphere. Even if it did, the most optimistic estimate of the
energy released through chromospheric reconnection is barely sufficient to
account for the coronal energy losses. Further, dynamical changes accompanying
reconnection between uni- and multi- polar fields are seen neither in the He I
data nor in narrow-band movies of the H alpha line core. We conclude that the
hypothesis must be rejected. Bright chromospheric, transition region and
coronal loop plasmas must be heated by mechanisms involving unipolar fields.
