  Context: The chromospheric anemone microflares, which were discovered by
Hinode satellite about a decade ago, are specific transient phenomena starting
from a few luminous ribbons on the chromospheric surface and followed by an
eruption upward. While the eruptive stage was studied in sufficient detail, a
quantitative theory of formation of the initial multi-ribbon structure remains
undeveloped until now. Aims: We construct a sufficiently simple but general
model of the magnetic field sources that is able to reproduce all the observed
types of luminous ribbons by varying only a single parameter. Methods: As a
working tool, we employed the Gorbachev-Kel'ner-Somov-Shvarts (GKSS) model of
the magnetic field, which was originally suggested about three decades ago to
explain fast ignition of the magnetic reconnection over considerable spatial
scales by tiny displacements of the magnetic sources. Quite unexpectedly, this
model turns out to be efficient for the description of generic multi-ribbon
structures in the anemone flares as well. Results: As follows from our
numerical simulation, displacement of a single magnetic source (sunspot) with
respect to three other sources results in a complex transformation from three
to four ribbons and then again to three ribbons, but with an absolutely
different arrangement. Such structures closely resemble the observed patterns
of emission in the anemone microflares.
