The large-scale flows may be at the origin of small sunspots and
pores.
Figure 3.
A fast moving sunspot, leaves the removed magnetic flux behind, which
is being picked up by the supergranular flows and displaced to the cell
boundaries, continue to move along the boundaries and slow down at
accumulation sinks and coalesce into a small sunspot. Figure 3
demonstrates this. The sunspot B was collected from the
magnetic fields of the sunspot A brought by the large-scale
flows, indicated by the arrows in the top-left image. The sunspot umbra
consisted of several pores which were pushed together, but they did not
inosculate into one umbra as bright umbral bridges, which marked
boundaries between the pores, were seen (image taken at 05:00:30 UT on
November 5).
It is worth noting that the evolution of sunspot B was a
competition between two parties: concentration of the magnetic flux by
converging motions and destruction of an accumulation sink. The sunspot
destruction was possibly connected with a rapid change of the sunspot
velocity, which made the accumulation sink unstable. The mean velocity
of the sunspot between Nov 3, 03:00 UT and Nov 4, 23:15 UT was about
0.08 km s-1. However, after 23:15 UT its velocity suddenly
increased up to 0.28 km s-1. The sunspot was completely
ruined by 15:00 UT on November 5. The arrows in the 07:30:30 UT image
show the directions in which pores moved after the sunspot was
destroyed.