  Using SDO/HMI and SDO/AIA data for sunspot groups of the 24th solar cycle, we
analyzed magnetic properties and He II 304 emission in leading and following
sunspots separately. Simultaneous examination of umbral magnetic properties and
atmospheric characteristics above the umbrae draws on average differences in He
II 304 contrast over the umbrae of leading and following spots we discovered
earlier for solar cycle 23 sunspot groups based on SOHO data as well as on the
hypothetical relationship between contrast asymmetry and magnetic field
asymmetry in umbrae. We use a more accurate and faster algorithm for solving
the pi-uncertainty problem of the transverse magnetic field direction in this
research producing new results on differences in magnetic field properties
between magneto-conjugated leaders and followers. We found that, in ~78% of the
cases, the minimum (over the umbra area) angle between the magnetic field line
and the normal to the solar surface, a_min, is smaller in the leading spots, so
the magnetic field there is more vertical than that in the counterpart
following spot. It was also found that umbral area-averaged angle <a> in ~83%
of the spot groups examined is smaller in the leader compared to the follower
and the maximum and mean magnetic flux densities inside the umbra depend on the
umbral area.
